text:
Low Gas Fractions Connect Compact Star-Forming Galaxies
to their z 2 Quiescent Descendants
Early quiescent galaxies at are known to be remarkably compact compared to their nearby counterparts. Possible progenitors of these systems include galaxies that are structurally similar, but are still rapidly forming stars. Here, we present Karl G. Jansky Very Large Array (VLA) observations of the CO(1–0) line towards three such compact, star-forming galaxies at , significantly detecting one. The VLA observations indicate baryonic gas fractions 5 times lower and gas depletion times 10 times shorter than normal, extended massive star-forming galaxies at these redshifts. At their current star formation rates, all three objects will deplete their gas reservoirs within 100 Myr. These objects are among the most gas-poor objects observed at , and are outliers from standard gas scaling relations, a result which remains true regardless of assumptions about the CO-H conversion factor. Our observations are consistent with the idea that compact, star-forming galaxies are in a rapid state of transition to quiescence in tandem with the build-up of the quenched population. In the detected compact galaxy, we see no evidence of rotation or that the CO-emitting gas is spatially extended relative to the stellar light. This casts doubt on recent suggestions that the gas in these compact galaxies is rotating and significantly extended compared to the stars. Instead, we suggest that, at least for this object, the gas is centrally concentrated, and only traces a small fraction of the total galaxy dynamical mass.
Subject headings:galaxies: formation — galaxies: ISM — galaxies: high-redshift
1. Introduction
Galaxies with large stellar masses ( ) and little ongoing star formation have been observed at redshifts up to (Straatman et al., 2014), and begin to appear in large numbers by (e.g., Kriek et al., 2006; Whitaker et al., 2010; Cassata et al., 2013). Many studies have shown that these early quiescent galaxies were much smaller at than equally massive star-forming galaxies at similar redshifts (e.g., Trujillo et al., 2007; van der Wel et al., 2014) or quiescent galaxies of similar mass in the local universe (e.g., Daddi et al., 2005; Trujillo et al., 2006; Buitrago et al., 2008; Cimatti et al., 2008; van Dokkum et al., 2008; Damjanov et al., 2011). With effective radii of just kpc, the stellar densities are of order 100 higher than present-day elliptical galaxies. Similarly massive and compact galaxies are extremely rare in the local universe (e.g., Trujillo et al., 2009; Taylor et al., 2010), implying significant size growth largely consistent with the effects of minor merging (e.g., Trujillo et al. 2011; Newman et al. 2012; see also Carollo et al. 2013). Although not all local massive galaxies had a compact progenitor (e.g., Franx et al., 2008; van Dokkum et al., 2008), most of the compact, massive galaxies likely now reside in the centers of present-day elliptical galaxies (e.g., Bezanson et al., 2009; Belli et al., 2014).
The formation mechanism(s) of the compact quiescent population is still unclear. Recently, however, a population of similarly compact yet highly star-forming galaxies at has been identified in deep Hubble Space Telescope imaging (Barro et al., 2013, 2014a; Nelson et al., 2014; Williams et al., 2014; van Dokkum et al., 2015). Given their structural similarity, these compact star-forming galaxies (SFGs) are natural candidate progenitors of the early quiescent population, requiring only the cessation of star formation to superficially match the stellar distribution and structure of the quiescent galaxies. Additional evidence from dynamical studies (Barro et al., 2014b; van Dokkum et al., 2015) and number density evolution (Barro et al., 2013) also indicates that compact SFGs will plausibly quench star formation on short timescales (500 Myr) to build up the growing quiescent population. The small sizes and non-exponential light profiles of compact SFGs present a clear contrast to the typical massive star-forming galaxies at , which consist mostly of gas-rich, rapidly rotating disks (e.g., Wuyts et al., 2011; Tacconi et al., 2013; Wisnioski et al., 2015), evidence which suggests very different evolutionary histories.
The aforementioned dynamical studies indicate that the stellar masses of compact SFGs are ubiquitously comparable to or somewhat in excess of simple estimates of the total dynamical masses, , determined through observations of . This implies that the dynamics of compact SFGs are almost completely dominated by the stars – any gas present likely traces, but does not significantly contribute to, the gravitational potential. van Dokkum et al. (2015) argue that the -emitting gas is likely rotating and more extended than the stellar light, preventing the unphysical scenario of . This inference was motivated by observations of velocity gradients across the slit consistent with rotation for a few objects. Although selection effects are likely in play, these observations imply that the gas is extended by a factor 2.5 relative to the stars on average. Adaptive optics-assisted integral-field or interferometric synthesis imaging can be used to spatially and spectrally resolve the gas, providing a more robust tracer of the dynamics than can be inferred from long-slit spectroscopy.
Recent cosmological simulations have matched the observed number counts of compact SFGs and quiescent galaxies (Wellons et al., 2015). This work suggests that the early quiescent population consists mostly of a combination of galaxies which formed their stellar mass early and remained compact since their formation time, and objects which have recently undergone gas-rich major mergers. High-resolution hydrodynamical simulations further indicate that many characteristics of compact massive galaxies can be reproduced through in-situ formation through gas accretion and cooling (e.g., Naab et al., 2009; Feldmann & Mayer, 2015), strong central star formation during a gas-rich major merger (e.g., Wuyts et al., 2010; Ceverino et al., 2015), and/or dissipative contraction of gas-rich disks (e.g., Ceverino et al., 2015; Zolotov et al., 2015). In each case, the properties of the gas are key, as its collisional nature allows energy to dissipate and angular momentum to be transferred through the galaxy, permitting the formation of characteristically dense stellar structures.
In this work, we present Karl G. Jansky Very Large Array (VLA) observations of the CO(1–0) line toward three compact SFGs at . CO(1–0) has long been known as a tracer of molecular hydrogen in the interstellar medium (ISM), the direct fuel from which stars form. If, as we have outlined above, the compact SFGs are in the process of quenching star formation to become quiescent galaxies, we may expect molecular gas properties unlike those of normal SFGs at these redshifts. In particular, if compact SFGs are to quench in tandem with the rapid buildup of the quiescent population, we expect short gas depletion or quenching timescales, indicating that the ongoing high star formation rates (SFRs) cannot be sustained for more than a few hundred Myr.
The outline of this paper is as follows. In Section 2, we describe our sample selection and VLA observations. Section 3 describes our results, including constraints on the molecular gas masses of our targeted objects (Section 3.1), gas fractions and depletion timescales (Section 3.2), and the physical extent of the molecular gas reservoirs in comparison to the stellar light (Section 3.3). We summarize our conclusions in Section 4. Throughout, we assume a flat CDM cosmology, with Mpc and (Planck Collaboration et al., 2015).
2. Data
2.1. Selection of Compact Star-Forming Galaxies
|Time On-Source
|Beam Size
We selected compact SFGs for VLA CO(1–0) observations from the van Dokkum et al. (2015) sample; detailed selection criteria for the parent sample of compact SFGs are available in that work. In brief, the objects were selected from multi-band photometric catalogs in the CANDELS fields from the 3D-HST program (Koekemoer et al., 2011; Brammer et al., 2012; Skelton et al., 2014; Momcheva et al., 2015) to be massive ( ), compact in WFC3 imaging (van der Wel et al., 2014), and star-forming in rest-frame UVJ color-color space. Catalog stellar masses were determined using stellar population synthesis modeling, and SFRs from UV+IR photometry assuming a Chabrier initial mass function, including Spitzer/MIPS 24 photometry to estimate the dust-obscured SFR of each object (Whitaker et al., 2012, 2014). These SFRs agree well with the 24 -based calibrations derived by Rujopakarn et al. (2013). Spectroscopic redshifts of each object were determined through Keck/MOSFIRE or NIRSPEC spectroscopy, detecting and [NII], and are accurate to . From the present sample, COSMOS 22995 is identified as an X-ray AGN, while the other two sources are not. We show the selection of compact SFGs in the SFR- (the so-called star-forming main sequence) and - planes in Figure 1, highlighting the VLA-observed objects and including later comparison samples.
From this parent sample, we selected northern targets for VLA CO(1–0) observations, preferring objects with high apparent SFRs. The SFR of each target, ranging from /yr in the 3D-HST catalogs, implied that they likely would not be detected in Herschel observations of the GOODS-N and COSMOS fields (Elbaz et al., 2011; Oliver et al., 2012; Roseboom et al., 2012). Indeed, only COSMOS 27289 was detected in any Herschel/PACS or SPIRE bands111Nelson et al. (2014) report detections of GOODS-N 774 in all PACS and SPIRE bands, but we are unable to reproduce their photometry using 24 cross-matched Herschel catalogs (Roseboom et al., 2012) or by visually inspecting the Herschel images. The flux densities reported as significant detections by Nelson et al. (2014) are comparable to or fainter than the quoted Herschel map depths. For consistency with the other sources and the 24 cross-matched catalogs, we treat this object as undetected by Herschel.. A simple modified blackbody fit to the FIR photometry indicates SFR /yr for COSMOS 27289, somewhat lower than its SFR in the 3D-HST catalogs. For the other two sources, the Herschel non-detections indicate upper limits on the obscured SFR of /yr, assuming K. These upper limits are consistent with the UV24 -derived catalog SFRs. For consistency in our own analysis and with van Dokkum et al. (2015), we use the 3D-HST catalog UVIR SFRs for all sources.
2.2. VLA Observations
VLA observations were carried out between October 2015 and March 2016 under programs 15B-283 and 16A-203 (PI J. Spilker), and are summarized in Table 1. GOODS-N 774 and COSMOS 22995 were observed in the VLA D-configuration (maximum baseline 1 km), while COSMOS 27289 was observed in the C-configuration (maximum baseline 3.4 km). Complex gain solutions were calculated using the quasars J1148+5924, J1008+062, and J0948+0022 for GOODS-N 774, COSMOS 22995, and COSMOS 27289, respectively, while observations of the quasar 3C286 were used both for bandpass and absolute flux calibration for all sources. The absolute flux scale is estimated to be accurate to 10%. In all cases, the correlator was configured to deliver 2 GHz of continuous bandwidth using the 8-bit samplers, with each baseband pair delivering eight dual-polarization basebands of 128 MHz width and 1 MHz channelization. The VLA Ka band receivers were tuned to center the CO(1–0) line in one of these basebands using the -based spectroscopic redshifts of van Dokkum et al. (2015).
After calibration, the data were imaged using natural weighting, which maximizes point-source sensitivity. No source is detected in 9 mm continuum emission, although we serendipitously detected a continuum source in the GOODS-N 774 data located at 12h36m22.50s, +6206'53.9". This source corresponds to GOODS-N 521 in the 3D-HST catalogs, and appears to be a galaxy. No lines are detected in this source, and we will not discuss it further.
Neither GOODS-N 774 or COSMOS 22995 are detected in CO(1–0) emission. For both sources, we extract the spectra shown in Figure 2 by fitting a point source to the visibilities averaged over 24 MHz (210 ), fixing the position to the source position in HST imaging, using the uncertainty from this procedure to estimate the noise in each channel. The noise is frequency-dependent due to the decline in sensitivity at the edges of each 128 MHz baseband delivered by the VLA correlator. We use these spectra to place upper limits on the integrated CO flux assuming line widths of 500 , given in Table 2.
COSMOS 27289 is significantly detected in CO(1–0) emission. A naturally-weighted integrated CO image of this galaxy is shown in Figure 3. To determine if COSMOS 27289 is spatially resolved in the C-configuration data, we fit a point source to the visibilities averaged over 100 centered at the peak of the CO emission. This velocity range encompasses 95% of the integrated CO emission. No significant residual emission remains. We also examined the visibility amplitudes of the channels with significant line emission as a function of baseline length and found no significant decrease on long baselines, consistent with pointlike source structure. Finally, we created other images of the data applying various tapers in the -plane. In each case, we recover the same integrated flux density as we measured from the full data. These tests indicate that COSMOS 27289 is not extended at 0.75" resolution, implying an upper limit on the CO size of kpc. We extract the spectrum shown in Figure 2 by fitting a point source to the visibilities averaged over 3 MHz (25 ), with the position fixed to the peak of the CO emission. We fit a simple Gaussian to this spectrum; the results are listed in Table 2.
|K pc
Note. – Stellar masses are from the 3D-HST catalogs (Brammer et al., 2012; Skelton et al., 2014), source sizes from van der Wel et al. (2014), and SFRs from Whitaker et al. (2014). We list 3 upper limits for the two non-detections, assuming a line width of 500 , approximately the median FWHM of the van Dokkum et al. (2015) sample. These values are equivalent to under the assumption of (K pc); see Section 3.1.
3. Results and Discussion
3.1. Molecular Gas Masses and the CO-H Conversion Factor
Central to our interpretation of the CO(1–0) observations is the conversion factor from CO luminosity to molecular gas mass, . The CO-H conversion factor is known to vary with the metallicity and kinematic state of the molecular gas (for a recent review, see Bolatto et al. 2013). For star-forming galaxies near solar metallicity, the value of ranges from 0.8 (K pc) in highly star-forming objects (e.g., Downes & Solomon, 1998) to 4 (K pc) in the Milky Way and nearby quiescently star-forming galaxies (e.g., Sandstrom et al. 2013; hereafter we suppress the units of ).
The appropriate value of in compact SFGs is not immediately obvious, but we can estimate its value and plausible upper and lower bounds through several methods. First, both the mass-metallicity relation and the [NII]/ line ratios of our sources indicate that the metallicity of each source is approximately solar or slightly super-solar (Pettini & Pagel, 2004; Mannucci et al., 2010). In this regime, variations in are no longer significantly affected by metallicity; instead, variations are driven by optical depth and/or excitation effects. This implies that is almost certainly not significantly higher than the galactic value, . Several authors have derived theoretical or empirical formulations of the dependence of on metallicity (e.g., Wolfire et al., 2010; Glover & Mac Low, 2011; Feldmann et al., 2012) which also indicate that is a reasonable upper limit for galaxies of approximately solar metallicity.
We can place further limits on by following the discussion of Narayanan et al. (2012b). These authors derived a fitting formula for using hydrodynamical simulations of isolated and merging systems coupled with line and dust radiative transfer. This fitting formula depends on both the galaxy metallicity and the CO surface brightness, where objects with higher CO surface brightness have lower conversion factors. For the two non-detections, we assume that the extent of the CO(1–0) emission is at least as large as the stellar emission seen in HST, which is nearly always observed (e.g., Tacconi et al., 2013; Spilker et al., 2015). This places an upper limit on the CO surface brightness. At solar metallicity, our two non-detections imply conversion factors 0.7. For COSMOS 27289, in contrast, our data place an upper limit on . In this case, because the CO(1–0) emission is unresolved at 0.75" resolution, the Narayanan et al. (2012b) fitting formula implies 1.6.
Finally, we can derive an empirical estimate of by noting that it appears to correlate well with galaxy SFR or (Spilker et al., 2015), based on a compilation of estimates of in objects using various techniques from the literature, including dust-based, dynamics-based, and CO surface brightness-based methods. For the objects in our sample, this correlation implies , in reasonable agreement with our previous estimates.
In summary, all indications are that the CO-H conversion factor is expected to be relatively low in these highly star-forming objects. For simplicity we adopt for the remainder of this work. For COSMOS 27289, this results in , and 3 upper limits of and for COSMOS 22995 and GOODS-N 774, respectively, integrating over a 500 line width (approximately the median FWHM of the van Dokkum et al. 2015 sample). We reiterate that these measurements carry significant systematic uncertainties, likely at least a factor of two. Future observations may help clarify the interpretation of CO(1–0) in compact SFGs by spatially and spectrally resolving the objects (yielding a dynamical constraint on ) or using observations of the long-wavelength dust continuum and dust-to-gas ratio arguments to derive alternate estimates of .
3.2. Molecular Gas Fractions and Depletion Timescales
Using the molecular gas masses derived in the previous section, in Figure 4 we compare the baryonic gas fractions of the compact SFGs with those derived for both normal, main-sequence galaxies (Daddi et al., 2010; Tacconi et al., 2013) and dusty, star-forming galaxies (DSFGs; compiled from Swinbank et al. 2010; Ivison et al. 2011, 2013; Fu et al. 2012, 2013; Magnelli et al. 2012; Magdis et al. 2012; Hodge et al. 2013; Ma et al. 2015; Aravena et al. 2016). Gas masses for all objects were derived from CO (although largely from higher-excitation transitions instead of the ground state in the main-sequence sample), and all measurements are subject to significant systematic uncertainties. From this figure it is clear that the compact SFGs in our sample are severe outliers from other populations, even though the compact SFGs generally lie near the star-forming main sequence (Figure 1; see also Whitaker et al. 2012; Barro et al. 2014b). With gas fractions 12%, the compact SFGs are among the most gas-poor objects observed at , in stark contrast to the high gas fractions ubiquitously observed at these redshifts (though see also Narayanan et al. 2012a). Even if we adopt a Milky Way-like , the inferred baryonic gas fractions are 30%, lower than 90% of the CO-observed comparison sample objects. In other words, the compact SFGs we have observed are genuinely deficient in CO emission, regardless of its conversion to .
A consequence of their low gas masses accompanied by rapid star formation is that the compact SFGs we have observed are similar outliers from main sequence populations in the Schmidt-Kennicutt relation between SFR and and in their gas depletion timescales, , as shown in Figure 5. In this respect, the compact SFGs appear analogous to the highly star-forming DSFGs, with depletion times yr. Whether the similar depletion times between compact SFGs and DSFGs is due to similar star-forming conditions in these objects is unclear. The low gas masses of compact SFGs indicate that they can undergo little further mass growth without replenishment of their gas reservoirs, in contrast to DSFGs, which have typical high gas fractions (Figure 4). The low gas fractions of compact SFGs seem to indicate that they are elevated relative to most objects on the Schmidt relation not because they exhibit very efficient star formation (high SFR at a given ), but because they are about to exhaust their gas reservoirs (low at a given SFR).
Some authors have suggested an evolutionary connection between DSFGs and the compact quiescent population (e.g., Blain et al., 2004; Tacconi et al., 2008; Toft et al., 2014) based in part on the observed small sizes of DSFGs (e.g., Simpson et al., 2015; Spilker et al., 2016). The low gas masses of compact SFGs indicate that they may be transitioning below the main sequence, perhaps shortly after the end of the submillimeter-luminous phase. Only 15% of compact SFGs are detected in Herschel/SPIRE images (Barro et al., 2014a), consistent with this interpretation. Unfortunately, we have essentially no constraint on the past star formation in these objects, making it difficult to know if the compact SFGs were once DSFGs.
In both gas fraction and depletion time, the compact SFGs are outliers by factors of 5 to 10 from standard gas scaling relations (e.g., Genzel et al., 2015), indicating that these relations are not applicable to this unusual population of galaxies. This result holds even if we adopt a galactic , in which case compact SFGs still have gas fractions 2 lower and depletion times 3 lower than massive main sequence galaxies. Taken together, Figures 4 and 5 indicate that the compact SFGs we have selected are indeed consistent with being the immediate progenitors of some fraction of the quiescent population, in a state of rapid transition. If the current SFR continues at its present rate with no further gas accretion, each object we have observed will deplete its gas supply before , presumably dropping below the star-forming main sequence at the same time. Our depletion time estimates could be lengthened if the SFR is declining and continues to decline as the gas supply is exhausted, but it is clear that compact SFGs can add very little additional stellar mass through star formation without substantial gas accretion.
The low measured gas fractions and short depletion times are consistent with the inferences made by Barro et al. (2014b), who noted that simple dynamical mass estimates are frequently close to or lower than the stellar masses inferred from population synthesis models, implying gas fractions 30%. A similar conclusion was inferred by van Dokkum et al. (2015), who estimated gas fractions 40%. Our results indicate even smaller gas fractions than estimated by these authors, affirming the conclusion that these galaxies have likely nearly exhausted their gas reservoirs and are either currently quenching or about to quench. The details of this quenching process are testable using higher spatial resolution observations. Observations of the dust continuum and high-resolution CO imaging would indicate whether the currently ongoing SFR and the reservoir of remaining gas are concentrated in the galaxy outskirts or the central regions. Such observations would provide a relatively straightforward test of theoretical models, which generally predict inside-out quenching (e.g., Zolotov et al., 2015).
3.3. A Compact Gas Reservoir in COSMOS 27289
We significantly detected CO(1–0) emission in COSMOS 27289, finding a line width FWHM of . The line observed by van Dokkum et al. (2015) was somewhat broader, (though note this line was only marginally spectrally resolved; the NIRSPEC instrumental resolution at this wavelength is ). If real, the difference in line width between CO(1–0) and may indicate that the CO-emitting gas is slightly more compact than the -emitting gas, or that the line is somewhat contaminated by nuclear emission. Our C array observations did not spatially resolve the source in CO. This implies an upper limit on the CO-emitting region of kpc. Our ability to distinguish velocity gradients is somewhat hampered by low signal-to-noise, but we similarly see no strong evidence for a gradient that would be consistent with a rotating disk or any other organized velocity structure. Across the line profile, the emission centroid changes position by 0.8" (7 kpc). In other words, our data offer no evidence that the CO-emitting gas is extended relative to the stellar emission ( kpc), and only weak evidence of different spatial distributions of the CO- and -emitting gas.
At least in this single case, our result contrasts with conclusion of van Dokkum et al. (2015), who inferred that compact SFGs host rotating gas disks which are more extended than the stellar distributions by an average factor of 2.3. This inference was motivated by noting that compact SFG gas velocity dispersions are systematically lower than expected from their stellar masses and sizes (equivalently, that stellar masses are higher than simple dynamical mass estimates), and supported by the observation that some objects showed velocity gradients across the slit consistent with rotation. For COSMOS 27289, the gas radius that reconciles the stellar and dynamical masses is 20 kpc (van Dokkum et al., 2015). At this large radius, the rotation curve implied by the stellar mass has fallen to match the low velocity measurement, but at the price of assuming that dark matter is negligible within 20 kpc. However, such a large gas radius would have been easily detectable in our data. For this object, invoking a large, rotating gas disk is not supported by the data.
How, then, can the discrepant dynamical and stellar mass estimates be reconciled? A simple, but unsatisfying explanation is that COSMOS 27289 is an outlier in terms of kinematic geometry or stellar mass estimate. depends on the assumed galaxy geometry and dynamics, resulting in factor of 2 systematic uncertainties. COSMOS 27289 may be an outlier compared to the assumed-disk-like overall population, or it may be that compact SFGs are not well-described by simple disk- or dispersion-dominated geometries (if, for example, they are generally recent merger remnants; Wellons et al. 2015). If COSMOS 27289 does have disk-like dynamics, it may be face-on, although its axis ratio in the rest-frame optical implies an inclination of 45 (van Dokkum et al., 2015). Second, we cannot rule out the possibility that stellar masses have been systematically overestimated in compact SFGs (but are accurate for most normal galaxies). If this is the case, the tension with the dynamical masses would be lowered while also bringing the gas fractions nearer to the value expected for normal, extended star-forming galaxies at this epoch. Given the extensive photometry and grism spectroscopy available for the extragalactic legacy fields in which compact SFGs have been selected, however, this seems unlikely.
A more likely solution is that the CO-emitting gas does not trace the full galaxy dynamical (or stellar) mass. The calculations of van Dokkum et al. (2015) required a very extended gas disk because of their assumption that the gas velocity dispersion must trace the full stellar mass of the compact SFGs – for a given dynamical model, if the total mass and circular velocity are fixed, the only remaining free parameter is the galaxy radius. Instead, our data paint a different picture. Given that the observed gas radius and velocity dispersion are small, the gas likely only traces a small fraction of the total galaxy mass in the central regions. In other words, instead of fixing the total mass and velocity dispersion to infer large radii, we argue that the mass interior to the gas effective radius is much lower than the full stellar mass, removing the need to invoke large gas disks to reconcile the stellar and dynamical masses.
In addition to our own data, this scenario is supported by the recent observations of Barro et al. (2016), who observed that the stellar absorption lines were nearly 70% broader than the gas nebular emission lines in a compact SFG at . This difference increases the dynamical mass inferred from the stars by nearly a factor of 3, and prevents the unphysical scenario of . A similar effect is likely at work in COSMOS 27289, predicting that future ultra-deep NIR spectroscopy will find a stellar velocity dispersion in excess of the gas velocity dispersion. More immediate progress may be made by continued CO observations using either higher-resolution B array observations or simply deeper observations with the current C array.
Having only detected and placed constraints on the dynamics of a single object, we cannot draw strong conclusions concerning the discrepancy between stellar and dynamical masses in the compact SFG population as a whole. While larger samples of objects with spatially and spectrally resolved spectroscopy will be required to investigate this issue further, it is clear that even relatively modest upper limits on the spatial extent of the molecular gas provide powerful constraints on the gas dynamics of compact SFGs.
4. Conclusions
We have observed the CO(1–0) transition in three compact star-forming galaxies in an effort to determine the amount of molecular gas in these objects. Our two non-detections and one detected source confirm low baryonic gas fractions and very short gas depletion timescales, as expected if compact SFGs are currently or on the verge of quenching star formation. The gas fractions and depletion times are much lower than predicted from gas scaling relations. In the detected galaxy, we see no evidence that the CO-emitting gas is spatially extended relative to the stellar light, and only weak evidence for a difference in the CO dynamics compared to the emission. This result demonstrates that invoking large gas disks to increase dynamical masses estimated from gas kinematics above the stellar masses may not be warranted. Instead, we argue that the gas is centrally concentrated, and therefore need not kinematically trace the full stellar mass of compact SFGs. An increased sample size and high-resolution follow-up observations of the molecular gas content of compact SFGs would indicate whether this is true of the bulk of the population or if COSMOS 27289 is an outlier.
- Aravena et al. (2016) Aravena, M., Spilker, J. S., Bethermin, M., et al. 2016, MNRAS, 457, 4406
- Barro et al. (2013) Barro, G., Faber, S. M., Pérez-González, P. G., et al. 2013, ApJ, 765, 104
- Barro et al. (2014a) —. 2014a, ApJ, 791, 52
- Barro et al. (2014b) Barro, G., Trump, J. R., Koo, D. C., et al. 2014b, ApJ, 795, 145
- Barro et al. (2016) Barro, G., Faber, S. M., Dekel, A., et al. 2016, ApJ, 820, 120
- Belli et al. (2014) Belli, S., Newman, A. B., & Ellis, R. S. 2014, ApJ, 783, 117
- Bezanson et al. (2009) Bezanson, R., van Dokkum, P. G., Tal, T., et al. 2009, ApJ, 697, 1290
- Blain et al. (2004) Blain, A. W., Chapman, S. C., Smail, I., & Ivison, R. 2004, ApJ, 611, 725
- Bolatto et al. (2013) Bolatto, A. D., Wolfire, M., & Leroy, A. K. 2013, ARA&A, 51, 207
- Brammer et al. (2012) Brammer, G. B., van Dokkum, P. G., Franx, M., et al. 2012, ApJS, 200, 13
- Buitrago et al. (2008) Buitrago, F., Trujillo, I., Conselice, C. J., et al. 2008, ApJ, 687, L61
- Carollo et al. (2013) Carollo, C. M., Bschorr, T. J., Renzini, A., et al. 2013, ApJ, 773, 112
- Cassata et al. (2013) Cassata, P., Giavalisco, M., Williams, C. C., et al. 2013, ApJ, 775, 106
- Ceverino et al. (2015) Ceverino, D., Sanchez-Almeida, J., Muñoz-Tuñon, C., et al. 2015, ArXiv e-prints, arXiv:1509.02051
- Cimatti et al. (2008) Cimatti, A., Cassata, P., Pozzetti, L., et al. 2008, A&A, 482, 21
- Daddi et al. (2005) Daddi, E., Renzini, A., Pirzkal, N., et al. 2005, ApJ, 626, 680
- Daddi et al. (2010) Daddi, E., Bournaud, F., Walter, F., et al. 2010, ApJ, 713, 686
- Damjanov et al. (2011) Damjanov, I., Abraham, R. G., Glazebrook, K., et al. 2011, ApJ, 739, L44
- Downes & Solomon (1998) Downes, D., & Solomon, P. M. 1998, ApJ, 507, 615
- Elbaz et al. (2011) Elbaz, D., Dickinson, M., Hwang, H. S., et al. 2011, A&A, 533, A119
- Feldmann et al. (2012) Feldmann, R., Gnedin, N. Y., & Kravtsov, A. V. 2012, ApJ, 747, 124
- Feldmann & Mayer (2015) Feldmann, R., & Mayer, L. 2015, MNRAS, 446, 1939
- Franx et al. (2008) Franx, M., van Dokkum, P. G., Förster Schreiber, N. M., et al. 2008, ApJ, 688, 770
- Fu et al. (2012) Fu, H., Jullo, E., Cooray, A., et al. 2012, ApJ, 753, 134
- Fu et al. (2013) Fu, H., Cooray, A., Feruglio, C., et al. 2013, Nature, 498, 338
- Genzel et al. (2015) Genzel, R., Tacconi, L. J., Lutz, D., et al. 2015, ApJ, 800, 20
- Glover & Mac Low (2011) Glover, S. C. O., & Mac Low, M.-M. 2011, MNRAS, 412, 337
- Hodge et al. (2013) Hodge, J. A., Carilli, C. L., Walter, F., Daddi, E., & Riechers, D. 2013, ApJ, 776, 22
- Ivison et al. (2011) Ivison, R. J., Papadopoulos, P. P., Smail, I., et al. 2011, MNRAS, 412, 1913
- Ivison et al. (2013) Ivison, R. J., Swinbank, A. M., Smail, I., et al. 2013, ApJ, 772, 137
- Koekemoer et al. (2011) Koekemoer, A. M., Faber, S. M., Ferguson, H. C., et al. 2011, ApJS, 197, 36
- Kriek et al. (2006) Kriek, M., van Dokkum, P. G., Franx, M., et al. 2006, ApJ, 649, L71
- Ma et al. (2015) Ma, J., Gonzalez, A. H., Spilker, J. S., et al. 2015, ApJ, 812, 88
- Magdis et al. (2012) Magdis, G. E., Daddi, E., Béthermin, M., et al. 2012, ApJ, 760, 6
- Magnelli et al. (2012) Magnelli, B., Saintonge, A., Lutz, D., et al. 2012, A&A, 548, A22
- Mannucci et al. (2010) Mannucci, F., Cresci, G., Maiolino, R., Marconi, A., & Gnerucci, A. 2010, MNRAS, 408, 2115
- Momcheva et al. (2015) Momcheva, I. G., Brammer, G. B., van Dokkum, P. G., et al. 2015, ArXiv e-prints, arXiv:1510.02106
- Naab et al. (2009) Naab, T., Johansson, P. H., & Ostriker, J. P. 2009, ApJ, 699, L178
- Narayanan et al. (2012a) Narayanan, D., Bothwell, M., & Davé, R. 2012a, MNRAS, 426, 1178
- Narayanan et al. (2012b) Narayanan, D., Krumholz, M. R., Ostriker, E. C., & Hernquist, L. 2012b, MNRAS, 421, 3127
- Nelson et al. (2014) Nelson, E., van Dokkum, P., Franx, M., et al. 2014, Nature, 513, 394
- Newman et al. (2012) Newman, A. B., Ellis, R. S., Bundy, K., & Treu, T. 2012, ApJ, 746, 162
- Oliver et al. (2012) Oliver, S. J., Bock, J., Altieri, B., et al. 2012, MNRAS, 424, 1614
- Pettini & Pagel (2004) Pettini, M., & Pagel, B. E. J. 2004, MNRAS, 348, L59
- Planck Collaboration et al. (2015) Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2015, ArXiv e-prints, arXiv:1502.01589
- Roseboom et al. (2012) Roseboom, I. G., Ivison, R. J., Greve, T. R., et al. 2012, MNRAS, 419, 2758
- Rujopakarn et al. (2013) Rujopakarn, W., Rieke, G. H., Weiner, B. J., et al. 2013, ApJ, 767, 73
- Saintonge et al. (2011) Saintonge, A., Kauffmann, G., Kramer, C., et al. 2011, MNRAS, 415, 32
- Sandstrom et al. (2013) Sandstrom, K. M., Leroy, A. K., Walter, F., et al. 2013, ApJ, 777, 5
- Simpson et al. (2015) Simpson, J. M., Smail, I., Swinbank, A. M., et al. 2015, ApJ, 807, 128
- Skelton et al. (2014) Skelton, R. E., Whitaker, K. E., Momcheva, I. G., et al. 2014, ApJS, 214, 24
- Spilker et al. (2015) Spilker, J. S., Aravena, M., Marrone, D. P., et al. 2015, ApJ, 811, 124
- Spilker et al. (2016) Spilker, J. S., Marrone, D. P., Aravena, M., et al. 2016, ApJ, 826, 112
- Straatman et al. (2014) Straatman, C. M. S., Labbé, I., Spitler, L. R., et al. 2014, ApJ, 783, L14
- Swinbank et al. (2010) Swinbank, A. M., Smail, I., Longmore, S., et al. 2010, Nature, 464, 733
- Tacconi et al. (2008) Tacconi, L. J., Genzel, R., Smail, I., et al. 2008, ApJ, 680, 246
- Tacconi et al. (2013) Tacconi, L. J., Neri, R., Genzel, R., et al. 2013, ApJ, 768, 74
- Taylor et al. (2010) Taylor, E. N., Franx, M., Glazebrook, K., et al. 2010, ApJ, 720, 723
- Toft et al. (2014) Toft, S., Smolčić, V., Magnelli, B., et al. 2014, ApJ, 782, 68
- Trujillo et al. (2009) Trujillo, I., Cenarro, A. J., de Lorenzo-Cáceres, A., et al. 2009, ApJ, 692, L118
- Trujillo et al. (2007) Trujillo, I., Conselice, C. J., Bundy, K., et al. 2007, MNRAS, 382, 109
- Trujillo et al. (2011) Trujillo, I., Ferreras, I., & de La Rosa, I. G. 2011, MNRAS, 415, 3903
- Trujillo et al. (2006) Trujillo, I., Feulner, G., Goranova, Y., et al. 2006, MNRAS, 373, L36
- van der Wel et al. (2014) van der Wel, A., Franx, M., van Dokkum, P. G., et al. 2014, ApJ, 788, 28
- van Dokkum et al. (2008) van Dokkum, P. G., Franx, M., Kriek, M., et al. 2008, ApJ, 677, L5
- van Dokkum et al. (2015) van Dokkum, P. G., Nelson, E. J., Franx, M., et al. 2015, ApJ, 813, 23
- Wellons et al. (2015) Wellons, S., Torrey, P., Ma, C.-P., et al. 2015, MNRAS, 449, 361
- Whitaker et al. (2012) Whitaker, K. E., van Dokkum, P. G., Brammer, G., & Franx, M. 2012, ApJ, 754, L29
- Whitaker et al. (2010) Whitaker, K. E., van Dokkum, P. G., Brammer, G., et al. 2010, ApJ, 719, 1715
- Whitaker et al. (2014) Whitaker, K. E., Franx, M., Leja, J., et al. 2014, ApJ, 795, 104
- Williams et al. (2014) Williams, C. C., Giavalisco, M., Cassata, P., et al. 2014, ApJ, 780, 1
- Wisnioski et al. (2015) Wisnioski, E., Förster Schreiber, N. M., Wuyts, S., et al. 2015, ApJ, 799, 209
- Wolfire et al. (2010) Wolfire, M. G., Hollenbach, D., & McKee, C. F. 2010, ApJ, 716, 1191
- Wuyts et al. (2010) Wuyts, S., Cox, T. J., Hayward, C. C., et al. 2010, ApJ, 722, 1666
- Wuyts et al. (2011) Wuyts, S., Förster Schreiber, N. M., van der Wel, A., et al. 2011, ApJ, 742, 96
- Zolotov et al. (2015) Zolotov, A., Dekel, A., Mandelker, N., et al. 2015, MNRAS, 450, 2327


text:
I. God made promises in the _______________.
A. A prophecy given by God is a _______________________ given by God.B. A prophecy fulfilled is God _______________________ His promise.
II. God ______________ all His past promises.
A. God's ____________________ promises can be trusted.B. Do not be weighed ______________.C. ____________________ God to keep His promises.

subset: commoncrawl


text:
Applications for 2018 are already open!
Dublin City University's Female High Fliers accelerator is a prestigious 13-week programme supporting Ireland's most promising female-led startups. The programme is run by the DCU Ryan Academy for Entrepreneurs who are already taking applications for 2018. Programme Director and COO of the DCU Ryan Academy, Niamh Collins joined Conall in the studio to discuss the programme. She was also joined Ciara Garvin, Founder of Workjuggle and Graduate of the High Fliers.
The tailored course is supported by Enterprise Ireland and attracts on average 130 high caliber female entrepreneurs every year.
Female Entrepreneurs can register for the 2018 programme via the following link: http://ryanacademy.ie/portfolio/female-high-fliers
To Listen to Niamh's interview on the Today FM's Sunday Business Show: Click Here


text:
Join our Brand Ambassador Program
Expand your single social circle. Date-Working mixers are the ultimate platform designed for professionals to meet, socialize and unwind in total style.
Speed Dating
Chemistry happens in person. Attraction happens in 30 seconds. Indulge in light convo and a dash of flirt during a series of mini dates at one of our events.
A one-on-one coffee, brunch or cocktails date, hand-picked by your matchmaker.
Service is now available in Montreal & Toronto.
Service is now available in Montreal & Toronto.
A Dashing Way to Date
We know dating is hard and meeting someone you like is even harder.
We're not saying that speed dating is the solution but Dashing Date's goal is to definitely make things a little easier for you. At our dating events, you will meet like-minded singles who share similar lifestyles. We are providing you, hands down, the most effective way to meet your next date, all the while enjoying a quality night out that is just as fun as being out with friends.
Click here to sign up as a member, it's free.
How Does It Work?
1. Become a member
Submit your member application via our sign up form. Look out for a welcome email from us
2. Pick 'n' Choose
Browse through upcoming Speed Dating and Date-Working events and select one to your liking
3. Date!
Enjoy an evening designed for singles to get to know each other through a series of speed dates


text:
Birds for Beer
You bring the beer, I'll bring the birds. (Birding from the slopes of the Turrialba Volcano, Costa Rica.)
Skip to content
Birds for Beer?
Around Turrialba
Bird banding at CATIE
Expeditions and Counts
In My Patch
Rare birds
Trips abroad
About Me
Contact Me
My Patch
My eBird
My Checklists
San Antonio Bird Checklist (My Patch)
CATIE Turrialba Bird Checklist
Espino Blanco Checklist
Tag Archives:
Blue dacnis
Great birding at Las Brisas – Part 1
Agami Heron and much more at Las Brisas in Limón province
Global Big Day
King Vultures and Scarlet Macaws at Ciudad Cortés
Privacy & Cookies: This site uses cookies. By continuing to use this website, you agree to their use.
To find out more, including how to control cookies, see here:
Cookie Policy


text:
Styrax benzoin is actually a tree that is native to some parts of South East Asia such as Laos and Vietnam and this bezoin is used for the preparation of an essential oil which is widely known for its medicinal purposes. Benzoin tree is quite tall and usually grows about 20 m of height and the leaves of this plant are oval in shape and also the flowers are merely greenish yellow in color.
It is known for its medicinal purposes since ages especially in places like Greece and some other areas of Europe. The oil is produced through a process called benzoin condensation where most of this oil actually consists of resin like substance. Apart from that it also contains compounds like benzxoin benzoate, benzoic acid, phenylethylene etc.
However it has to be noted that there can be certain allergic conditions with the usage of this oil and hence it has to be kept in mind that benzoin essential oil has to be tested before the usage. Doing so might keep you away from various health problems on the whole. In this regard, this article vividly features some of the best health benefits of benzoin essential oil which makes you to include it in your regular diet.
1. Used As A Deodorant:
The name itself suggests that benzoin essential oil is rich in aroma and hence it can be used in the preparation of perfumes and deodorants. One mustn't forget that benzene is actually a cyclic organic compound and is aromatic in nature and this is the reason why benzoin produces aroma. Also one stunning advantage of this essential is that this can be used both to remove the body odor as well as a room cleaner. This is because of the fact that when benzoin essential oil is applied to the body it actually attacks the germs that causes odor. However many of the people doesn't prefer to use it directly instead they feel it a lot worthy to include a tint of oil in bath water as well as massage oils. At times, women even use this oil to smoke their hair to make it smell a lot better.[1]
2. Diuretic In Nature:
One of the prominent uses of benzoil oil is that it actually acts as a diuretic and this is nothing but it actually facilitates the production of excess urine. Production of excess urine is necessary at times because urine can be probably the only way where some of the unwanted toxins and other harmful substances move out of the body. This removal of wastes is highly necessary as the storage of these harmful substances might result in various infections as well as some other deadly diseases on the whole.[2]
3. Controls Diabetes:
Diabetes has now become one of the most alarming issues nowadays and this is because unlike the previous generations, diabetes has been striking many of the individuals at some very early ages and there is a lot of necessity to control the growth of this deadly disease. This is because extreme cases of diabetes might also be fatal at times and this isn't a case expected and hence one has to opt for suitable natural remedies to handle the cases of diabetes as prolonged use of synthetic medicines might get you to land in troubles completely. Benzoin essential oil can be highly helpful under such cases.
This is because of the fact that this essential oil is highly necessary for the reduction in the glucose levels in an individual in the blood and this in turn reduces the effect of diabetes. Also certain properties of benzoin essential oil are known to promote the secretion of insulin from the endocrine glands of the body and insulin is something that can keep the sugar levels in your blood in control.[3]
4. Gum Health:
It has become quite a natural process to get the gums weaken at some very early ages. This is solely due to the fact that the food habits of the humans have changed a lot and also the quality of the food has been continuously decreasing nowadays. Hence it is highly important to care of your oral health with the help of certain natural remedies that can be highly helpful in handling the cases of gum disorder and reduce the extent of bleeding of gums. This is something highly desired and hence it is recommended to all the individuals who are actually suffering from various gum problems to use this essential oil as a natural mouthwash daily and this induces sound oral health to the individual.[4]
5. Skin Health:
Benzoin essential oil is known well to handle certain skin diseases and this is solely due to the fact that certain compounds in the oil have some high anti inflammatory properties. Hence this can be used to handle the cases of some skin problems especially wounds and scars that are formed due to some heavy wounds.[5]
6. Antidrepessant:
Many of the studies ave proved that benzoin essential oil is highly necessary to keep the mood in control and this has also a tendency to take you out of some bad mood. This is because of the fragrance it generates and also certain other compounds that assist a lot in maintaining your mental health. Hence it is highly recommended by a few doctors that benzoin essential oil has to be highly used during some cases of depression, stress and even anxiety.[6]
7. Reduces Acidity:
One of the main advantages of benzoin essential oil is that it actually keeps the acidity in check where acidity is solely the main reason for many of the gastric problems.[7]
8. Used As Antiseptic:
Certain properties of benzoin essential oil makes it a worthy alternative that handle the cases of wounds quite well and also strive a lot to reduce the wounds to the maximum extent.[8]
9. Vulenary:
This property of benzoin essential oil makes it a worthy one as it protects the wounds from various infections.[9]
10. Anti Inflammatory:
The anti inflammatory nature of benzoin essential oil is highly responsible to handle the cases of some deadly diseases and also reduces the extent of ulcers as a whole.[10]


text:
By: Newsroom Staff on 10 Aug, 2017 14:38
CELTIC are delighted to announce that Shaun Maloney has returned to the club, taking up a role as a development coach with the Under-20s. The 34-year-old, who previously enjoyed two playing spells with the Hoops, has now finished his career as a player, and will begin coaching with the U20s.
Shaun, a graduate of the Celtic Youth Academy, spent seven years at Celtic between 2000 and '07 before moving down south to join Aston Villa. He returned to Paradise in 2008 and spent three further years with the Hoops.
In total he made 215 appearances for Celtic, scoring 52 goals and winning five league titles, five Scottish Cups and three League Cups. He gained 47 caps for Scotland, while he also enjoyed spells with Wigan Athletic, Chicago Fire and Hull City.
Everyone at Celtic welcomes Shaun back to the club and wishes him every success in his new coaching role.


text:
Hey, there, M.D. This is the perfect computer desk for examining patients in either a standing or sitting position (or something in between). It boasts a steel base, lockable casters, and easy adjustment to meet your rapidly changing needs. Pick from an espresso, walnut, cherry, black, or white finish.
Its dimensions are 27.5" W X 19" D X 28-42" H.


text:
In many ancient cultures, a BULL is considered as a symbol of strength, virility, valor and magnanimity.
Even in modern times, the upward trends in stock markets are symbolised as BULLish trading patterns.
Our BULL sculpture is an ideal gift to all those Alpha males who like to take their challenges head-on !!
Made from high quality brass, this one definitely adds a classic and contemporary look to your work desk or a showcase.
- The sculpture is sold in a flat state that will be folded by the customer. No tools are necessary for folding bull's body. You may use pliers for bending bull's nose.
BULL - Brass Origami
Package size: 220X173X5 mm / 8X 6.9X0.2 Inches
Flat state size: 196X167X1.5 mm / 7.7X 6.6X0.06 Inches
Folded Bull size: 148X90X58 mm / 5.8X 3.5X2.3 Inches
Material: brushed brass with handmade finish (All Wallabies are hand-finished. Therefore, minute finishing differences between products may occur.)
Cleaning: Wallaby products are made of uncoated natural metals. Therefore, and like other metals, they might tarnish over time. It's a natural process. To remove tarnish, use brass cleaners only. Other cleaning agents can damage the products. When using a new cleaner, please test it on a small, inconspicuous area first.
For indoor use only.


text:
Breakups can seem like the end of the world when they have just happened, but in the long run they can bring new forms of happiness. This is true in both life and music. There are times when a band's breakup leads to the creation of another one equally as fantastic, if not greater than the first. This leads us to the topic of this week's 3 Of The Week. Songs by bands that emerged from the fall of another band.
1. "L'Via L'Viaquez" – The Mars Volta
At the risk of losing credibility, I will go out and say that I prefer The Mars Volta over At the Drive-In. Sure it may not be the scenester thing to say, but I truly believe it. If anyone thinks that At the Drive-In was crazy, then they have not heard The Mars Volta, who are downright insane. It only takes one listen of "L'Via L'Viaquez" the 12 minute long epic from the band's second release Frances the Mute (surprisingly it's not even the longest song on the album). "L'Via L'Viaquez" shows the mastery of guitarist Omar Rodriguez-Lopez, who is an insanely creative guitarist, as he packs technicality, funkiness, and a sweet dose of Mexican music influence in this one track, which is accompanied by his partner in crime, frontman Cedric Bixler-Zavala, who pulls off notes that most vocalists in the world wish they could hit, and alternates from singing in English and Spanish, making the song much more unique. While it may sound like a chore on paper, listening to this 12 minute long track is far from one. At the Drive-In's breakup may have saddened many who saw the band as the next savior of mainstream music, but there's no denying that we got a pretty amazing outfit out of it.
2. "Dark Blue" – Jack's Mannequin
North and Leaving Through the Windows may have been the soundtrack to the highschool days of every romantically misunderstood kids in the early 2000s, but after their breakup frontman Andrew McMahon made sure to continue providing his lyrical support to the teenagers of the second half of the decade. "Dark Blue" is exactly what you want from the band that rose from the ashes of Something Corporate, very piano driven, as it should be expected from a song written by McMahon, and given its beauty thanks to McMahon's crisp and clear voice, but what truly makes this song shine is the lyrics, which shows that McMahon understands you more than anyone will. "Dark Blue" and the rest of Everything In Transit were meant to be your soundtrack, and I'll be damned if there's a single teenager who doesn't relate to the lyrics in this wonderful album.
3. "Clint Eastwood" – Gorillaz
Before 2001, did anyone ever think that Damon Albarn, who at the time was mostly known for being the frontman of Blur, would replicate the success of Blur with Gorillaz? When the band was announced music fans everywhere might have thought Albarn had gone insane; an animated band that mixed Britpop with Hip-Hop? There was no way that could work. Leave to Albarn to prove critics wrong. "Clint Eastwood" the first single of their 2001 debut self-titled is the prime example of the success of Gorillaz. Reaching #4 on the UK Singles Chart "Clint Eastwood" had shown that Gorillaz had the star power to reach the mainstream audience, but luckily the music also backed up its success. Mixing Damon Albarn's singing with Del Tha Funkee Homosapien's rapping may seem like a strange idea on paper, but it works wonderfully. Accompanied with a keyboard line straight out of a horror film, and a harmonica part that evokes the illusion of a western, the music showed that the band had what it took to be more than a mere vanity project. Gorillaz was a weird but wonderful experiment coming from the brain of the same man who had previously brought us Blur, and "Clint Eastwood" was only the beginning of the madness that Gorillaz would become.


text:
Contact: Kaithy Chen | Sales Manager (Overseas) phone:+86-769-8809 8086 WeChat:kaithymini2013 address:Room 201~204, ShangJia Urban Industrial Park, No. 83, FenXi Rd, WanJiang District, DongGuan, GuangDong, China (Postal Code: 523055)
Health knowledge of dust free cloth
source: release time:2017-12-29 Hits:565
A new type of fiber product with softness, breathability and plane structure is formed directly through the use of polymer chips, short fibers or filament through all kinds of mesh forming and consolidation technology.
Non-woven fabric (also called nonwovens) is a new generation of environmentally-friendly materials. It has the characteristics of water repellency, breathability, flexibility, no combustion, no poison, no irritation and rich color. If the material is placed outside, it will decompose naturally, and its longest life span is only 90 days. It will decompose indoors and decompose within 5 years. When burning, it will be innocuous, tasteless, harmless, and will not be any residual substance, so that it will not pollute the environment, so environmental protection will come from it. It is suitable for washing and other points. It has the characteristics of short process, high output, low cost, fast variety change and wide source of raw materials. According to the different production processes, non-woven fabrics can be divided into:
1, wet dustless cloth: it is to separate raw materials into fibers in water medium, and make different fiber materials mixed to make fiber suspension slurry, and suspend slurry to transport into mesh forming mechanism.Fiber will be reinforced into cloth under wet condition.
2, spunlaced nonwovens: high pressure tiny water flow to a layer or multi-layer fiber network, so that fibers intertwined together, so as to strengthen the fabric and have a certain strength.
3, hot metal nonwoven fabric: it refers to fiber or powdery hot melt adhesive reinforcement in the fiber net, and then the fiber net is reinforced by heating and melting to reinforce the cloth.
4, the pulp air flow into the net non-woven cloth: also can be called as dust free paper, dry paper non-woven fabric. It uses airflow net forming technology to break wood pulp fiberboard into single fiber state, and then uses airflow method to make fiber agglomerate on net curtain, and then reinforce the fabric into cloth.
5, spunbonded dustless cloth: after the polymer has been extruded and stretched to form continuous filament, the filament will be laid into mesh, and the mesh will be transformed into non-woven fabric through its own adhesion, thermal bonding, chemical bonding or mechanical reinforcement.
6, melt spray non-woven fabric: its process process: polymer feeding - melt extrusion - fiber formation - fiber cooling - Network - - reinforced into cloth.
7, non-woven cloth is a kind of dry non-woven, non-woven needle puncture needle is the effect of fiber net, fluffy reinforcement into cloth.
8, stitched woven non-woven fabric: one is dry non-woven fabric, and stitching is reinforced by warp knitting coil structure, such as mesh, yarn layer, non-woven material, such as plastic sheet, plastic thin metal foil or their combination, to make non-woven fabrics.
Recommended ProductsMORE+
- About purge mop 2017-12-29
- What is a dustless cloth 2017-12-29
- What is the sole cleaning machine 2017-12-29
- Clean room network view the clean industry will usher in gold development in the next ten years 2017-12-29
- Look around! Four principles to resist particles into the clean room workshop! 2017-12-29
- Dust free fabric - Anti - static super clean fabric and ordinary anti - static fabric 2017-12-29


text:
Mrs. Stephanie Irene Rehnert, 56, of Franklin Township, Pa. passed away Monday July 9th in Carbon County. She was the wife of Robert M. Rehnert. They were married for 24 years last Aug. 14th 2017. Born in Albuquerque, New Mexico on Sunday, May 13, 1962, she was a daughter of Earlene (Winter) Stinnard of Honesdale, Pa. and the late Lester Stinnard Sr.. She was currently employed as an independent jewelry consultant. She was of the protestant faith. Stephanie was involved with Lehighton community activities and previously volunteered her time as a Girl Scout leader in the local community. She enjoyed sewing, needlepoint, and loved her family oriented activities. Surviving in addition to her husband are 3 daughters, Erin M. wife of William J. Hill III, Cassandra T. Rehnert, Alexandra C. Rehnert of Lehighton, a son, Ryan J. Bortree of Honesdale, Pa. a grandson, Taegan Bortree, a sister, Daphanie, wife of Timothy Ellis of Honesdale, a brother, Lester Sinnard Jr. of Honesdale, nieces & nephews. A Celebration of Life Service in her honor will be held on Monday, July 16th at 7 p.m. at The Ovsak FH, 190 S. 4th St., Lehighton with the Reverend Jennifer K. Eckhart officiating. Call 5-7 p.m. on Monday at the funeral home. The interment will be private. Memorial Contributions in her honor may be made to Girl Scouts of America at GSUSA Fundraising, P.O. Box 5046, New York, NY 10087. Online condolences can be offered at www.ovsakfh.com
To send flowers to the family or plant a tree in memory of Mrs.Stephanie Irene (Stinnard) Rehnert, please visit our floral store.


text:
In a shocking revelation, Busola Dakolo, wife of super star singer, Timi Dakolo has disclosed how pastor of Commonwealth of Zion Assembly, popularly known as COZA raped her at 17.
The mom of 3 revealed this to Chude Jideonwo, a Nigerian lawyer, journalist and media entrepreneur in a video which has now gone viral.
Busola who said she came home on holiday, while in secondary school then, recounts how her sisters convinced her to join the church which was formerly known as Divine Delight Club where Christians gather to share the word of God on Saturdays.
She further alleged that Pastor Biodun Fatoyinbo was married with a child when he came to her house one early morning, raped her and told her she should be happy he was the one who took her virginity.
Before now, there have been rumours that the man of God sleeps with members of his church, but none has been bold enough to publicly open up.


text:
COVID-19 update: We're open for business!Due to supply issues, we may be limited on some inventory.
We appreciate your patience during this challenging time
Track your order here! »
This 48" high x 1/8" thick high-density foam will provide a protective barrier between your new liner and the pool wall. Wall foam helps protect your liner from rust and corrosion and it will improve your pool's heat retention. Help keep your liner like new for years to come with wall foam!
NOTE: Spray Adhesive not included.
|More Information
|Pool Size
|21' Round


text:
Collaboration Quote of the MonthDecember 28, 2010
Leave a Comment » | Collaboration Quote of the Month | Tagged: collaboration, cooperative, Era of Collaboration, quotes, sustainability, working together | Permalink
Posted by Shanie Matthews
"I Am Only A Child" Youtube Video Example that Children Know More than Our GovernmentsDecember 21, 2010
Why is it that a young girl can speak so eloquently about global challenges that we as adults stumble over?
1 Comment | Those Collaborating | Tagged: collaboration, cooperative, Era of Collaboration, global warming, I am only a child, sustainability, working together | Permalink
Posted by Shanie Matthews
Surfrider Foundation Teams Up with Protect Our WintersDecember 14, 2010
The Surfrider Foundation, the leading name in beach and coastal protection, has teamed up with Protect Our Winters, the top non-profit from the world of snow sports to offer a combined membership that will allow boardsports enthusiasts to protect where they play.
Founded three short years ago, Protect Our Winters has quickly established itself as the leading environmental voice in the snow sports industry. During that time the group has successfully worked to place several solar energy projects in rural communities, appeared before Congress on Capital Hill, and inspired the environmentally-themed film project "Generations."
For over twenty-five years the Surfrider Foundation has led in beach and coastal protection. As the original and largest non-profit in the action sports community, Surfrider Foundation has been instrumental in keeping our coastal waters clean through their Blue Water Task Force program, and protecting world-class beaches and breaks such as Trestles from development.
"We couldn't be more thrilled to be teaming up with Protect Our Winters," says Surfrider Foundation CEO Jim Moriarty. "This is a great opportunity for outdoor enthusiasts to support two great organizations in protecting our playgrounds, be they sea or summit."
To be a part of the action, Protect Our Winters / Surfrider Foundation is offering a dual membership for just $40 annually – a $5 savings off buying both memberships separately.
Leave a Comment » | Those Collaborating | Tagged: collaboration, cooperative, Era of Collaboration, Protect Our Winters, sustainability, The Surfrider Foundation, working together | Permalink
Posted by Shanie Matthews
Bu Dongwei, Former Prisoner of Conscience, Asks All to Write For Other's Rights and Help Prevent TortureDecember 4, 2010
In the evening of May 19, 2006, six to seven police suddenly broke into my home. They searched everywhere. But all they found were several books – words on paper.
These books were used as "evidence" against my activities as a practitioner of the Falun Gong spiritual movement, which is banned in China.
Possession of these books led to my torture and persecution inside a Chinese labor camp for two and a half years.
The Chinese government tried to use these words on paper to imprison me, but it was your words on paper that helped set me free.
Your letters will stay in my heart forever.
Send a letter of hope and make a difference in someone else's life, as many of you did in mine.
My personal case is a witness – your letters make a difference.
I felt the attitude of the guards change toward me for the better when your letters came in. Although I did not see the letters when I was in the labor camp, I knew that I was not alone. The guards knew that Amnesty International and its supporters stood behind me.
From my experience, I know that the attention and pressure from the international community can help improve the conditions of jailed people.
Write for Rights is an important action. Only through the joined efforts of upright and kind people, like you, can we stop the injustice in the world.
Please say that you'll Write for Rights now. Your words can open prison doors. They can stop torture and prevent executions. Your words can make a difference.
Thank You,
Bu Dongwei
Former prisoner of conscience
**Amnesty International is asking that people send the letters between December 4 – 12 to make a collaborative statement.
Leave a Comment » | Those Collaborating | Permalink
Posted by Shanie Matthews


text:
It's that time again! Jim Cramer rang the lightning round bell, which means he gave his take on caller favorite stocks at rapid speed:
Weight Watchers Intl: "No, I have to tell you I think they've be outmoded by connected fitness, which is why I remain a fan of Under Armour. Only buy half now because I do think we are in a tough market."
Maxlinear Inc: "I had David Aldrich from Skyworks Solutions on the show, and you come to me with Maxlinear? It's up a lot, I would ring the register there and go right into Skyworks."
Infinera Corp: "A very good digital equipment provider. Very good. I have to tell you and let me say it—Cisco is now down a lot before it reported that upside quarter. How about a little yield, and a nice stable base?"
El Pollo Loco: "El Pollo Loco is el pollo bad-o. What's the matter with Chipotle? Chipotle reported the good quarter. Chipotle is doing really well. Just because it has a $745 handle? Come on, let's step up to the big time."
Tractor Supply Company: "Tractor supply is constantly jammed, that is a niche retailer that I like very much. I say stick with it."
ResMed Inc: "Interesting company, don't see a catalyst for this sleep deprived problem. This has always been a company that people think is going to get a takeover bid, and I am not a buyer of a company just because I think it's going to get a takeover bid."
Illumina Inc: "I see you with Illumina, and I raise you with Thermo Fisher Scientific....But let me tell you, Thermo Fisher, Marc Casper [CEO] I think he delivers. That is what I want to be in."
Read more from Mad Money with Jim Cramer
Cramer Remix: Wrong way to play a big market trend
Cramer: Housing can't carry us through China chaos
Cramer: Stop hoping for a Twitter takeover!
Cypress Semiconductor Corporation: "This thing has just been a total house of pain. They are doing everything right, we had T.J. Rodgers on, they had a big quarter and he's a big owner of it, it's got a yield at 4.5 percent. I don't know what to say, other than this market is a little bit irrational when it comes to semiconductors."
Amicus Therapeutics: "They have some very niche interesting drugs for some really unmet needs. We have looked at FOLD and we think it is a good stock. Remember, it is a speculation, but it is a good spec."
Questions for Cramer?
Call Cramer: 1-800-743-CNBC
Want to take a deep dive into Cramer's world? Hit him up!
Mad Money Twitter - Jim Cramer Twitter - Facebook - Instagram - Vine
Questions, comments, suggestions for the "Mad Money" website? firstname.lastname@example.com


text:
Answer on @Quora How is Javascript used within the Spotify desktop application? : JavaScript on top of C++ which handle files retrievals but JS handles GUI
Answer by Mattias Petter Johansson:
I would bet that the Spotify desktop client is among the top 25 most intricate uses of JavaScript in the world. The Spotify desktop client UI is completely built with JavaScript, resting on top of the same C++ core that the iOS and Android clients uses. The C++ core is responsible for things like playback, providing offline editing of playlists and local files, but rendering and interacting with the UI is handled by JavaScript. The communication between the C++ parts and JavaScript is done through a simple messaging interface simply called bridge. The UI itself is HTML/CSS, which is generated by Handlebars and LESS.
Spotify is internally divided into small (3-12 people) teams called squads. A feature is generally owned by a single squad, and during normal conditions the squad has all it needs to develop and maintain its feature. It's normal for a squad to have iOS, Android, web, and backend developers under its roof. The general idea is that every squad should have the ability to work on its feature pretty much on its own, minimizing the need for the squad to ask other parts of the organization for permission and/or help.
The latest versions of all Spotlets are zipped and bundled with the desktop client binary on every release, assets and all. However, we can also live-deploy new versions of the apps into the running clients of users. This is very useful for emergency releases, but we can also release Spotlets to certain user groups, such as employees or designated testers only. We can even release apps that aren't originally bundled with the client, which is very handy during our hack weeks, allowing us to quickly get apps into the hands of non-techie decision makers in the company. After demoing your thing, you end off with "and now type this uri into the search field of your desktop client, to try it out with your own account!". This whole system was originally invented as part of the now-defunct Spotify Apps initiative, to support third-party developers adding functionality to the client.
While teams are autonomous, there is functionality that we all would like to share because we explicitly want it to work the exact same way in all apps. For instance, we have a CSS framework called GLUE. It was originally a fork of Twitter Bootstrap, but we've diverged heavily from that over time. Generic functionality such as some list and buttons, we also provide shared components for, but it's very easy for squads to just just templates, or just partially use functionality from the shared frameworks. It's important that squads are able to control their own reality and can pick the best solution for their problem domain, instead of having a company tool forced down their throats just because it's in-house.
We use npm extensively. We have our own internal npm repository where we publish internal modules, and we package the code together using a Browserify-like tool. npm has been magnificent for us. For the browser-specific testing, we use Mocha and PhantomJS.
If you like my writing, don't miss out on more of it –
follow me on Quora and Twitter (http://twitter.com/mpjme)
How is Javascript used within the Spotify desktop application?


text:
De goede wetenschapper (in Dutch) – Luca Consoli & Ron Welters (red.)
This bundle is in Dutch. Het bedrijven van goede wetenschap gaat over meer dan alleen het correct toepassen …
A farmer's son goes to university to study agricultural sciences. But once there he becomes fascinated by linguistics, gains his doctorate in that subject and finds a job as a lecturer. Outgrowing his own family background along the way, he marries the wrong woman. At work he proves no match for his sophisticated colleagues and his career is unspectacular. But he believes in the importance of his subject and endears himself to his students. Those around him barely acknowledge that, however, and he leads a lonely life.
This book provides a revealing insight into the important role of intrinsic motivation in science. That can make people extraordinarily single-minded, to the extent that they sublimate their own interests. Which may appear admirable to outsiders, but can also foster behavioural characteristics bordering on the autistic.
Available at bol.com
NRIN devotes a great deal of attention to the website's content and would greatly appreciate your suggestions of documents or links you believe to belong on this website.
This selection is an incomplete convenience sample, and does not reflect NRIN's vision or opinion. Including an item does not necessarily mean that we agree with the authors nor does it imply we think unmentioned items are of poorer quality.
Please report any suggestions, inaccuracies or nonfunctioning hyperlinks etc. that you discover. Thanks in advance!Contact


text:
Le Jour Watches
Founded in the 1960s, Le Jour watches is a brand that specializes in using unique engineering techniques and fine-quality materials to create truly one-of-a-kind timepieces. Taking inspiration from leisure sports and activities such as sailing, yachting, aviation and auto-racing, Le Jour watches have a sporty appearance while still retaining an elegant look in an effort to bring the world of luxury timepieces and durable sports watches into one timepiece style. Though the original Le Jour brand fell to the wayside thirty years ago, Le Jour has been born anew, taking over where it once left off to bring the same quality and sophistication to today's market as it did decades ago.
Le Jour has introduced two watch collections: the Mark I and the Vintage Divers. The Vintage Diver collection is characterized by its SL C3, Green SuperLumiNova luminescent hands and indices, 300-meter water resistance, stainless steel case and anti-reflective lens for visibility in any light setting. The Mark I line features the same luminescent features but has subdials on the main dial as well to offer a sportier, more efficient way to keep the time. The Vintage Divers utilize an ETA 2824 Swiss Automatic movement to keep the time, while the Mark I line uses an Automatic Chronograph 7750 ETA Valjoux movement.
The Independent Mid-Tier Watch Brand Le Jour watches can be found on their website and at the authorized European dealer WatchBandit, ranging in price from $800 to $1,250. Each one comes available with shipping to anywhere in the world.
Gruppo Gamma Watches
Aiming to reinvent the classic watch styles of the 1940s, Gruppo Gamma has come up with the Vanguard line of timepieces, which put an imaginative spin on the styles of old. The Vanguard Retro takes cues from the styles of yesteryear, while the Vanguard original offers a fresh, modern spin on the timepiece.
The first watch on the menu is the Gruppo Gamma Vanguard, the watch that puts an imaginative twist on the classic timepiece. Featuring a large case that measures 44 millimeters in diameter, the Vanguard has a slim profile with a bold appearance and an eye-catching presence on the wrist. The case comes in your choice of either marine-grade phosphor bronze or surgical stainless steel, both of which are every bit as durable as the other and able to protect the watch even with frequent wear. Both styles are also resistant to water as deep as 200 meters. A self-winding ETA 2824-2 Swiss movement inside of the timepiece accurately keeps the time.
With the Vanguard Retro timepiece, all of the specs are the same, with the only main difference being the style of the dial itself. The dial of the Vanguard Retro is inspired by old-fashioned watch dials with either its blend of index styles or bulbous Roman numerals. Protecting the dial is sapphire crystal glass that protects against nicks and scratches. Both of these watches are available on the Gruppo Gamma site and at the authorized European dealer WatchBandit and can be purchased for prices between $750 and $950 depending on the watch you choose.
Meccaniche Veneziane Watches
The Arsenale Automatic Watch from Meccaniche Veneziane takes its inspiration from the Serenissima Republic of Venice's Royal Shipyard, a shipyard that was constructed many years ago. The Arsenale Automatic Watch is one that takes its cues from the vessels and the merchant ships that found a home in this shipyard, with their finishes even being directly tied to the way these ships were created, right down to the construction of the submarines and other naval vehicles.
The Arsenale Automatic Watch features a case which is made out of 316L stainless steel measuring 45 millimeters in size, making them large and legible. The hands as well as the indices are all diamond cut. These dials have been protected by domed sapphire glass, able to resist any sort of nicks, scratches or dents in order to ensure a watch that is able to last a lifetime. These Arsenale Automatic Watches have Cal. MV044 movements inside of them keeping the time. The movements are modeled after the Miyota 821A movements, those of which are mechanical movements made in Japan. The straps that come with these Arsenale Automatic Watches from Meccaniche Veneziane are made from genuine, handcrafted Italian leather for a luxurious finish. There will soon be launched a new version of the Arsenale watch from.
Sekford Watches
Sekford Watches were created upon a singular belief: utilize the craftsmanship seen in traditional timepieces, but implement a modern spin that makes them more accessible to today's society. Though other timepiece manufacturers seem to take note of only the global watchmaking trends, Sekford is different in the way that they take inspiration from their own corner of the globe. They bring classic British watchmaking techniques into the manufacturing process of their sleek dress watches while incorporating contemporary aesthetic elements that make them perfect for any modern person.
This watch company has named itself after Sekforde Street that is found in Clerkenwell, London, that was once the home of the most important and well-recognized watchmaking locations in the world. Thereby, Sekford took their inspiration from the watches that could be found in this hub, inspired by the traditional, dedicated craftsmanship to be found there. With their modern appeal, these watches have transformed from solely classic designs to ones with minimalist visual appeal in the form of abundant white space and crisp fonts.
The Independent Mid-Tier Watch Brand Sekford Watches believes that watches should be timeless, yet always accessible to the modern age. They focus on beauty and quality above all else by employing expert craftsmanship skills into each watch they produce. These watches are built to last, not only with their durable materials but in the world of fashion as well. Made with the highest quality materials, Sekford timepieces are perfect for any formal occasion and are to be worn by those with a modern aesthetic encompassed by a flair for the traditional.
Bravur Watches
An independent watch brand based in Stockholm, Sweden, Bravur is the dream of two friends come to fruition. The watch brand launched in 2011 with the goal of creating watches that give you a touch of elegance in any situation, from adventures at home to around the world. The Geography Series is a line of watches designed specifically for travel, thanks to the unique features while still being sophisticated with classic Bravur style details.
With the Geography Series, you can be sure you are getting the most out of your travels both in terms of style and functionality. What makes these Geography Series timepieces stand out from others is the additional dial and the extra hand that will allow you to keep track of not just one but two time zones in the world. The series delivers all of the characteristics you have come to expect from the beautiful Bravur watch designs such as recessed, two tone dials and their overall appearance.
Each one of these watches is fashioned out of top quality stainless steel, complete with a sapphire crystal backing on the case to make it stronger. On the tips of the hands is Superluminova material that allows you to check the time in the dark at a glance. Inside, reliable Swiss movements tick away the seconds on both time zones. Find these watches on the Bravur website and enjoy free shipping on both Geography Series styles.


text:
Your cartThere are no more items in your cart
Hiking mouse, Big sister
It may be complemented with Maileg collection furniture and clothing (size Micro), also available. Also with the camping tent, the Book House for mice and the wooden houses.
Check HERE the size guide for Maileg's soft toys, clothes and furniture.
Maileg collections are characterized by a unique and delightfully traditional style. The products are of exquisite quality.
- color
- 100% Cotton
- Dimensiones
- 12 cm
- Color
No reviews
Customers who bought this product also bought:
All products
Baby mice twins in box
All products
Giftwrap Happy birthday
All products
Happy Camper Tent, Mouse
All products


text:
When I lie dead
What will they remember?
My cold heart?
My carelessness and carefree ways?
I doubt that
Those who will remember me, at all
Will remember the smiles
Those of mine, and those I brought
The smiles and the many written lines
Which often meant more to me than to them
I will be remembered as a giver
Often giving more than I had
They say this is a character flaw
I'd say that's right
But, in the end
That's just me
And I can't (and won't) speak for them
I hope some of these many interactions
Have sat well, with them
© D J Loweman 2015


text:
I ACTUALLY did this. I ACTUALLY made it all the way through 365 consecutive days of parkour training without stopping. It wasn't always very >good< training, and I definitely feel I phoned some days in when things got dire, but I DID do it. Guys, I'm genuinely astonished by this. I know I keep bringing it up, but I'm not sure any of you really realize how dramatically unprecedented all of this is for me. It had literally never crossed my mind to do something like this before. Ever. In the whole 34 years of my life leading up to my decision to do this last year, it never once occurred to me that I might be capable of intentionally, and relentlessly practicing one thing every day for an entire year. Especially not something athletic.
But wait! There's more! I'M DOING IT AGAIN!
I finished one set of 365 days and then got up the very next day and started the counter over again. I didn't even give myself a whole 24 hours to let the first set sink in. I just got up and started over as if this were now the most self-evident thing in the world. I guess it's become a lifestyle now, or something. To the date of this post, I'm 69 days into a second year of American Parkour's 365 challenge.
Let me be real honest with you, though. This is really hard. It isn't supposed to be easy, though, and it isn't always going to be fun. It wouldn't be a challenge if it were, would it? But most of the time it is fun, if you choose to let it be, and sometimes it's just what I need in a day. Sometimes it's the only thing that holds me upright. But I think the first thing you need to understand about doing something like this if you've never done one before, is truly that it's going to be hard. Probably a lot harder than you think. But here's the thing – it IS possible.
I pushed myself to do this last year through sickness, extreme stress, exhaustion, debilitating depression (sometimes this challenge was the only thing I managed to not fail to do in a day except get out of bed and eat), a wildly fluctuating schedule, really odd environments, and a handful of injuries. I badly broke a toe during a wall run ten days in last year and sat down on our couch afterwards and cried because I thought I was done, and because I was angry with myself. I couldn't see how I was supposed to continue if I couldn't even walk properly. But the moderators encouraged me to expand my thinking and hang in there. They gave me some ideas and that's what I worked with until I was gradually able to ease back into higher-impact things. That taught me a lot. Possibly more than the entire rest of the year. If I could find a way to keep training through what seemed like a critical injury, what – realistically – could possibly keep me from making it through whatever else the year had in store? Nothing. After that, I knew nothing was going to stop me. And it didn't.
The rest of the year took me on a winding road through adventure, whimsy, success, failure, joy, and frustration. It put me into much closer contact with myself, and also with a whole lot of other people and my surroundings. I met friendly dogs, curious passersby, intrigued children, and fascinated adults. I got a middle aged man from our previous apartment building to do a safety vault, even though he didn't think he could, bonded with a neighborhood kid over pop vaults (which I swear he thought was magic), and spent an hour helping three young girls get a feel for rail walking. Sometimes strangers cheered me on, too. I once had a small audience rooting for me while I worked up the courage to make a big jump, and on another occasion, received respect and encouragement from a random jogger.
"We believe in you! You can do it!" said the audience before I leapt from a low roof.
"That's a pretty impressive jump!" Said the jogger, after I'd gone from the edge of a landscaping box forwards and a little upwards to the edge of a bench. "Whatever you're doing, keep going!"
Both of those moments of unexpected encouragement were really well-timed. I was pushing my limits on both counts.
Doing the APK365 last year also taught me a lot about my own capacity for creativity, resourcefulness, and discipline. I had to get real inventive some of the time, and a lot of the time I needed to put on some metaphorical spurs and give myself a harsh heel. I now have a dramatically better sense of my own learning process, too. I now know what works for me, and what doesn't, and what I need in order to stay motivated through rough patches. I know more about where my mental and physical strengths lie, and what things I need to work on.
There have been mental and visible physical benefits as well. Even though I didn't always push myself as much as I could have, I gained noticeable amounts of muscle. Particularly in my upper body, which feels really good for someone who's never really had much upper body strength. I crossed paths with a guy last spring who struck up a friendly conversion with me over – of all things – a small fire he witnessed me putting out. I'd watched someone else throw a lit cigarette butt into a landscaping box full of wood chips and bury it. Rather than going out, the cigarette smoldered and the chips caught the flame and I happened to be there and had water. This guy stopped, I think, because of the smoke, but lingered and started to chat. I don't remember what came before this, but after a while he looked at me and said "You look a woman who can take care of herself". For someone who's spent her whole life being underestimated, perceived as a target, and treated as if she's made of glass, that's a life-changing victory. It was easily one of the most meaningful compliments I've ever been given because it made it very clear that there's been a distinct shift in how people perceive me, even when they know nothing about me, or my activities. That's a shift I've been waiting my whole life to see happen. I've never perceived myself as being delicate, but it seems as though most of the rest of the world generally has, and now that's finally changing. The image of myself I've always felt exists on the inside, but has been trapped behind a tangle of labels and scars is finally beginning to break through. Around the holidays, my mother commented that she thought I'd grown taller. At 35, that's very unlikely to be true. But maybe it's my spirit that's grown taller. Maybe I hold my head up higher and face the world squarely rather than hunching and cowering slightly like a mistreated animal waiting to be whipped again.
Have there been any negative repercussions? A few, I suppose. The toe I broke didn't heal properly and will probably never function normally again. There's a very real chance I'll eventually break it a second time. I've gained a handful of shin scars – the telltale mark of the traceur -, took a few sprains of varying severity, and experienced shin splints for the very first time in my life. Plus, of course, a whole lot of bruises, scrapes, minor strains, and tissue inflammation. But these are all relatively superficial things that anyone is likely to get doing almost any sport, and honestly, I'm kind of proud of those scars. They show that I've been willing to truly challenge myself and have not let those painful moments stop me.
This year, I'm working hard to make sure I'm really challenging myself and growing as much as possible. I really, really love that feeling of facing a challenge, either mental or physical, and then breaking it, so that's what I want to reach for as much as I can this year. Last year, the my focus was on simply completing the challenge itself. I didn't know if I was capable of producing a full 365 consecutive days of movement. Now that I know I can, it's time to raise the bar, because that's the philosophy parkour teaches. Mindfully feel out and test your limits, set your goal bars slightly beyond them, figure out what you need to strengthen, and then – when you obtain those goals – move the bar up. I feel I'm off to a pretty good start. Now that I've got a better foundation of strength and body awareness, I'm finally able to begin pushing my technical limits and expanding/strengthening my skills.
I'm also currently working on applying the mindsets and philosophy I've been learning through parkour to rapier fencing. I burned out of fencing really badly about a year and a half ago. I hit a major plateau and got so agitated and frustrated that I came very, very close to completely quitting. I really love rapier, though, and after five years of effort, I didn't want to simply drop it and walk away, so I opted to take an extended break from it through almost all of last year. Thanks to that time off, and to this challenge, I'm now properly equipped with the tools and understanding I need to resume my rapier training and blow through that blockage.
A few people have asked for advice on how to stick a challenge like this out. Here are a few of my thoughts:
- Make sure the parameters of your challenge are very clear. If you're not doing it as part of an organized group, take time to hash out – in detail – what will and will not count. Set the bar to something that's a genuine challenge, but is still attainable. Then, relentlessly hold yourself to them. Understand that you might need to be a little harsh with yourself and will probably need to dig deep for reserves of resilience that you've possibly never needed before.
- Pace yourself. Remember that you don't need to press the pedal to the mat every single day in order to make progress. Ask yourself 'What do I most need for today? What level of energy am I capable of giving today? What can I do – today – that's constructive?' It's a marathon, not a dead sprint. If you try to go 100% every day and refuse to allow yourself 'rest days', you're very likely to burn out and/or do more damage than good.
- Figure out what your 'bare minimum' is for days when things are critically rough, either mentally, physically, or both. Do this before those days occur so that when they come, you can simply do them and not lose more energy trying to figure out what to do. And then, when it happens, accept that it's happening and don't attempt to fight it. Tell yourself 'I just need to make it through >insert applicable time or task goal<. That's all I need for today. Just that much', and then be willing to accept that that's all you can give that day. You can lean in harder again on another day, when you've got more gas in the tank.
- Be absolutely honest and clear with yourself about why you are doing what you're doing, and why it's worth this much work. You'll need to know this when you begin to question your resolve and I promise, you will. Knowing exactly why you're reaching for this, and what you're hoping to get out of it will give you something solid to stand on. It will be the knot at the end of your rope.
- Be willing to flex and adapt. It's unrealistic to think that you will be able to do the same thing at exactly the same time every single day for an entire year. Sometimes you're going to need to adjust. Take advantage of whatever opportunity a day presents and know that you're going to need to make the challenge a priority every day. You might need to accept that you're going to need to let some other thing on your list go in order to make room for this. Planning ahead also really helps. If you know what your schedule for the following day is likely to look like, take a moment the night before to plan when you'll complete your challenge.
- Consider the value of accountability. You don't necessarily have to be really visible and public about it. You just need a friend who's willing to hold you accountable and check in. Better still is if someone will do it with you, or do their own 365 along side you so that you can cheer each other on and share experiences.
- Try to keep your activity from becoming a repetitive chore. Add creative elements, look for new challenges, change the environment you're doing it in, do something silly, make it fun and engaging. Make it a thing you want to do most of the time, rather than a thing you have to do. Alternately, find a way to make the activity meditative by doing it very mindfully. That might mean doing it slowly, or being very aware of your movements and the sensations they're bringing you.
- If you start to feel overwhelmed, try setting specific goals for yourself within the larger challenge. Focus on building up, or achieving a particular thing, or set of things over the course of a week, or a month. Don't think about the whole year all at once. Take it one day, or week, or month at a time, and look at how far you've come, rather than how far you still have to go.
Also – Check out this awesome 2018 recap video that my friends over at American Parkour were kind enough to put together for me!
If you'd like to follow this year's APK365, look for the group "APK Parkour 365 2019" on Facebook, or watch the threads #apk365 and #apk3652019 on Facebook and Instagram.


text:
Today I love Mixed Doubles Curling and, SPOILER ALERT, the fact that Canada won gold at the Olympics for this event making them the world leader with more Olympic gold medals in Mixed Doubles Curling than any other country in the world with a total of one of them. Yay Canada. I love that I think that is funny. I also love that someone brought up the topic of trying to fix the Olympics and my mind instantly went to creating more new events, like luge moguls, team pursuit four man bobsleigh, and downhill slalom relay races. I also love crokicurl though I've never played it and I'm just now realizing that if you've never heard of crokinole you won't have any idea what I'm talking about, but you should google crokicurl, you can thank me later. I love that I have been up a while because I'm still not over the jet lag stuff and have a hard time staying up as late as I normally do. I love that there was curling on when I got up and it was the aforementioned gold medal mixed doubles game so we watched it. I love that we're going to try playing doubles curling in a couple of weeks and I love that there might be a league starting up at my club so I'm keeping my fingers crossed for that.
Today I love that I have a busy week ahead of me, with meetings and jobs to do and lunch appointments and other grown up stuff and whenever that happens I always get a picture of myself as a little boy in a baggy oversized suit with pant legs and sleeves too long and a briefcase that almost drags on the floor. I love that I've had a couple of ideas for songs lately and it would be nice to see the end of that long drought.
Today I love that there is strawberries in the porridge. I love that we have cooked enough food to last several days and I love leftovers so that's a double love thing. I love that the consensus is that the current quantity of flour in the pantry is sub par and so we've decided to get new flour and use the stuff we have for sauces and bread in the bread-maker only … maybe try it for pie crusts and see what happens. I love when there is household agreement on things and that seems to happen a lot in this house. I love that there are many things coming up in the near future that could be called adventures.
Today I love coffee and being able to sip it leisurely in front of the TV while John and Kaitlyn throw rocks for gold.


text:
One more bounces off the rim, and KSU loses to Toledo, 67-64
Two games in a row Kent State has had a chance to reach overtime with a long three-point shot at the buzzer.
Two games in a row the shots — both by redshirt freshman Tyra James — have bounced off the rim.
You certainly can't blame the loss on James' shot. It was 22 feet away, low percentage at best.
It was things early in the game — eight fouls in the first quarter, 10 turnovers on the first half, and 1-for-17 three-point shooting for the game — that kept KSU on the losing end of a a 67-64 score to Toledo.
The Flashes are now 4-17 on the season, 1-10 in the MAC. Toledo is 12-, 7-3 in the conference.
There was a lot of good in the game against one of the better teams in the conference. KSU came from eight points down at halftime to tie the game 49-49 at the end of the third quarter. They stayed within four points of Toledo most of the fourth quarter, and if a Jordan Korinek layup hand't rolled off the rim with 1:03 the go, it might have been different.
After Korinek's miss, KSU was forced to foul, and Toledo's Brenae Harris made two fouls shots. The Flashes got within 65-64 when Larissa Lurken snatched an airball from McKenna Stephens and threw it in and converted a three-point play.
But Harris made two more foul shots, and James' last-second shot didn't go in.
"The biggest difference (between the two halves) was that players committed themselves to the board," coach Danny O'Banion said after the game, "and we took better care of the basketball."
KSU outrebounded Toledo 20-15 in the second half and outscored them 17-10 on second-chance points. The Flashes held their turnovers to six in the second half.
Led by Korinek, the Flashes outscored Toledo 42-16 in the paint.
The Rockets won the game at the foul line — where they were 17 of 20 — and on three-pointers. Their three-point percentage wasn't great — 29.6 percent — but they made eight when KSU could hit just one.
Kent State jumped to a 9-0 lead, but Toledo came back, mostly on nine straight free throws. Fouls put Korinek, Kent's leading scorer, in trouble in for most of the last three quarters.
Still, the 6-2 sophomore scored 23 points on 9 of 13 shooting and 5 of 6 foul shots. She had seven rebounds in 29 minutes.
"I'm very proud of Jordan," O'Banion said. "That was about as much adversity as she's had in fouls this season, and she stayed aggressive and engaged. She showed more patience and was effective in the point (when she had four fouls)."
- Lurken had 13 points and six rebounds. She was 5 of 15 from the field and 1 of 7 from three-point distance. She had six turnovers.
- Walk-on freshman Paige Salisbury started her fourth straight game — all among KSU's best performances of the year. She had four points, two assists and equaled her season high in turnovers — all of two —in 34 minutes. The 19 points Toledo scored off turnovers had little to do with her.
- Sophomore McKenna Stephens had perhaps her best game as a Kent State player. She scored 12 points on 6 of 11 shooting and led the team with eight rebounds. She had two assists and a block in a career-high 33 minutes.
- The Flashes got a good six minutes out of 6-4 freshman Merissa Barber-Smith, who scored four points on 2 of 2 shooting and blocked a shot.
- After playing a man-to-man defense for most of the game at Miami Wednesday, KSU returned to its match-up zone for most of the night. It was as effective as it's been this year.
KSU has a week off before it hosts the MAC West's best team, Ball State, next Saturday.
Other MAC scores:
- Akron (12-10, 6-5) 77, Miami (9-12, 3-7) 65, at Akron.
- Ohio (18-4, 10-1) 95, Northern Illinois (9-12, 2-8) 70, at Ohio.
- Ball State (16-5, 8-2) 59, Buffalo (11-10, 3-7) 57, at Buffalo.
- Central Michigan (15-7, 9-2) 76, Bowling Green (8-11, 4-5) 75, at Bowling Green.
- Eastern Michigan (14-8, 5-6) 70, Western Michigan (13-10, 5-6) 66, at Eastern.