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PROBES-I: A Compendium of Deep Rotation Curves and Matched multiband Photometry

We present the Photometry and Rotation Curve Observations from Extragalactic Surveys (PROBES) compendium of extended rotation curves for 3163 late-type spirals, with matching homogeneous multiband photometry for 1677 of them. PROBES rotation curves originally extracted from Halpha long-slit spectra and aperture synthesis HI (21cm) velocity maps typically extend out to a median 2R_e (or 1R_{23.5, r}). Our uniform photometry takes advantage of GALEX, DESI-LIS, and WISE images and the software AutoProf to yield multiband azimuthally averaged surface brightness profiles that achieve depths greater than 25 mag/arcsec^2 (FUV, NUV), 27 mag/arcsec^2 (g, r), and 26 mag/arcsec^2 (z, W1, W2). With its library of spatially resolved profiles and an extensive table of structural parameters, the versatile PROBES data set will benefit studies of galaxy structure and formation.


INTRODUCTION
Galaxies are some of the best laboratories for studying fundamental questions about cosmology, dark matter, black holes, and more. They are also complex objects with detailed physics occurring on scales spanning many orders of magnitude, and evolving in diverse environments, making the exercise of identifying the drivers of galaxy structure and evolution especially challenging. Teasing out and modelling evolutionary and transformative processes such as star formation (Salpeter 1955;Tojeiro et al. 2009;Conroy 2013), merging (Toomre & Toomre 1972;Naab et al. 2014), dust attenuation (Holmberg 1946;Burstein & Heiles 1984;Tully et al. 1998;Stone et al. 2021a), and angular momentum transport (Lin & Pringle 1987;Obreschkow & Glazebrook 2014) has deepened our understanding of the development of structure in the universe, while opening many new questions.
Corresponding author: Connor Stone connor.stone@queensu.ca * Released on September 22, 2022 Chief among those, the elusive dark matter cannot be directly observed and must be inferred (Faber & Gallagher 1979;Bertone & Hooper 2018;Wechsler & Tinker 2018), despite its considerable effect on the evolution of galaxies. The mismatch between the mass distribution through spatially resolved kinematic and photometric profiles is certainly one of the strongest evidence of dark matter in galaxies (Bosma 1978;Faber & Gallagher 1979;van Albada & Sancisi 1986;Courteau et al. 2014). While galaxy photometry is rather easily acquired, with large deep multi-wavelength imaging programs covering most of the sky (York et al. 2000;Skrutskie et al. 2006;Lawrence et al. 2007;Lang 2014;Bianchi et al. 2017;Dey et al. 2019;Ivezić et al. 2019), kinematics are more challenging given the targeted approach and time-consuming integrations, with most studies limited to a few hundred systems (Rubin et al. 1980;Mathewson et al. 1992;Courteau 1997;Sofue & Rubin 2001). Some recent programs have yielded large samples of galaxy kinematics with spatially resolved integral-field spectroscopy, though rarely reaching depths beyond ∼R e (SAMI: Croom et al. 2021), ∼1.5R e (MaNGA: Bundy et al. 2015), or ∼ R 23.5 (CAL-IFA: Sánchez et al. 2016). These efforts are nonetheless commendable and the future mapping of gravitational potentials in galaxies will require deep spatially resolved kinematics for tens of thousands of galaxies to achieve statistical power.
In this study, we take a step in this direction by providing one of the largest catalogues of galaxy light profiles and major-axis rotation curves (hereafter RCs) in the form of the "Photometry and Rotation Curves Observations from Extragalactic Surveys (PROBES)" compendium. PROBES combines some of the largest existing surveys of spatially resolved major-axis rotation curves (hereafter RCs) into a single homogenized compilation of 3163 spiral galaxies. We have taken advantage of the GALEX Survey (Bianchi et al. 2017), DESI Legacy Survey (Dey et al. 2019), and the unWISE survey (Lang 2014) to compliment the kinematic information with homogeneous multiband data from the UV to the NIR in the FUV, NUV, g, r, z, W1, and W2 bands. With this publication, we make the PROBES compilation readily available to the community.
The PROBES combination of deep photometry and kinematic information for a large number of spiral galaxies is ideally suited for studying the interplay between baryons and dark matter. The PROBES sample has already been included in various studies during its development. Stone & Courteau (2019) examined the Radial Acceleration Relation of PROBES galaxies, favouring a ΛCDM interpretation over Modified Newtonian Dynamics (Lelli et al. 2017). PROBES galaxies also allowed Stone et al. (2021a) to find that scatter had been systematically underestimated in previous analyses of galaxy structural scaling relations. PROBES scaling relations have been used as a benchmark for the analysis of MaNGA data Arora et al. (2021) and to characterize the diversity of spiral galaxies Frosst et al. (2022). This paper is divided as follows. Sec. 2 introduces the surveys amalgamated into the PROBES compendium, emphasizing the respective selection criteria. A variety of structural parameters extracted from the light profiles and RCs for these galaxies are then presented in Sec. 3. The data tables and readme files provided with the PROBES compendium are described in Sec. 4. We conclude in Sec. 5 by reiterating the usefulness of these data for studies of galaxy structure and formation, stellar populations, galaxies as cosmological tracers, and more.

Sample Selection
The PROBES compendium is a combination of seven previously published RC surveys with new FUV, NUV, g, r, z, W1, and W2 matched photometry presented here, combined and homogenized for easier usability. Brief descriptions of the seven surveys, with an emphasis on sample selection 1 , are presented below. Most of the original surveys provided their own photometry in addition to the RCs; however, for homogeneity, we have extracted and standardized our own photometry from the DESI-LIS (Sec. 2.5), unWISE (Sec. 2.6), and GALEX (Sec. 2.7) surveys instead. Of the 1677 PROBES galaxies with r-band photometry, > 99% have g, z, W1, and W2 bands while 80% have FUV, NUV bands. While DESI-LIS and unWISE images enable detailed studies of their respective spatially resolved light profiles, the noisier GALEX images will only be used to compute global quantities such as total luminosities and to complement spectral energy distributions (SEDs).
2.1.1. Mathewson 1992Mathewson et al. (1992 published Hα RCs for 827 spiral galaxies found largely in the southern hemisphere. Galaxies were selected primarily from the ESO-Uppsala catalog (Lauberts 1982(Lauberts , 1998) with morphological types shown in Fig. 1, diameters greater than 1.7 arcmin, heliocentric recessional velocities below 7, 000 km s −1 , moderate inclinations, and Galactic latitude |b| > 11 deg. Some galaxies were taken from other surveys (Mathewson et al. 1992). The velocity uncertainties for these RCs were not reported, instead we use the residuals from our model fits (see Sec. 3.2.2) to estimate reasonable upper bound uncertainties.
2.1.2. Mathewson 1996Mathewson & Ford (1996 expanded the Mathewson et al. (1992) sample to 2017 spiral galaxies with Hα RCs primarily located in the southern hemisphere. The morphological distribution is shown in Fig. 1. However, not all objects in Mathewson et al. (1992) were included in Mathewson & Ford (1996). As in Mathewson et al. (1992), velocity uncertainties for RCs were not provided and a model fit was used to determine upper bound uncertainties (see Sec. 3.2.2). The sampling criteria were similar to those of Mathewson et al. (1992), though with higher heliocentric recessional velocities in the range 4, 000-14, 000 km s −1 and apparent diameters between 1.0 − 1.6 arcmin. Once again, a small number of galaxies were taken from other surveys, such as the Catalogue of Galaxies and Clusters of Galaxies (Zwicky et al. 1961;Zwicky & et al. 1995).
2.1.3. Courteau 1997 The Courteau (1997, hereafter C97) sample is a survey of 353 late-type galaxies with Hα RCs and morphological types shown in Fig. 1. These were collected largely for cosmic flow studies for which systematic and random velocity uncertainties were of great interest (Courteau et al. 1993). Thus, many galaxies have multiple measurements, with some having as many as four repeat RCs, and well characterized velocity uncertainties. For the PROBES compendium, all multiple RC measurements, were stacked as described in Sec. 2.4. The sample was selected from the Uppsala Catalog of Galaxies (Nilson 1973;Lauberts 1998) and the catalog of cluster galaxies from (Bothun et al. 1985). C97 galaxies were selected to have Hubble types Sb-Sc, Zwicky magnitude m B ≤ 15.5 (see Giovanelli & Haynes 1984), blue Galactic extinction less than 0.5 mag (based on Burstein & Heiles 1984), inclinations between 55 − 75 deg, blue major axes less than 4 arcmin, no interactions or mergers, and no bright foreground stars (Courteau 1996).

SCII 1999
The all-sky survey of Dale et al. (1999, hereafter SCII) offers Hα RCs for 602 galaxies in 52 Abell clusters up to heliocentric recessional velocities of 25, 000 km s −1 . Galaxies were selected from the Abell Rich Cluster Catalog (Abell et al. 1989), favoring those with redshift information available at the time. Morphologies for the SCII galaxies are shown in Fig. 1. These galaxies add a significant number of late-type cluster member galaxies to the PROBES compendium, allowing for environmental studies among others. We use the velocity errors as reported in the original data.

Shellflow 2000
The Shellflow survey (Courteau et al. 2000) of 186 spiral galaxies was designed to study an all-sky shell in redshift space to measure a cosmological bulk flow of galaxies with high precision. The Shellflow sample geometry meant that a large fraction of the galaxies could be observed from both northern and southern hemisphere observatories, namely the Kitt Peak National Observatory and Cerro Tololo Inter-American Observatory, thus mitigating calibration errors from different instrumentation. The Shellflow sample was selected from the Optical Redshift Survey of Santiago et al. (1995). Galaxies were chosen to be noninteracting and of morphological types indicated in Fig. 1, with heliocentric recessional velocities between 4, 500 − 7, 000 km s −1 , inclinations between 45 − 78 deg, AB extinctions less than 0.3 mag (as determined by Burstein & Heiles 1982), and no bright overlapping foreground stars or tidal disturbances. We use the velocity errors as reported in the original data.

SPARC 2016
The Spitzer Photometry and Accurate Rotation Curves (SPARC) sample compiled by Lelli et al. (2016) is an amalgamation of over 50 smaller samples totaling 163 galaxies with a mix of Hα and HI RCs. Approximately one-third of the SPARC galaxies have hybrid HI and Hα RCs to combine the higher spatial resolution provided by Hα with the extensive radial extent of synthesis HI radio maps, where available. The distance estimates for SPARC galaxies rely on a number of methods, including Hubble flow, tip of the red giant branch, Cepheids, Ursa Major cluster distance, and supernovae. All distances and their uncertainties are reported in the SPARC survey, and we use them directly in the PROBES compendium. The sample was carefully chosen to have a range of morphology, luminosity, and surface brightness (SB) from the limited selection of galaxies with HI measurements (Lelli et al. 2016). We use the velocity errors as reported in the original data.

SHIVir 2017
The Spectroscopy and H-band Imaging of Virgo Cluster Galaxies (SHIVir) survey presented in Ouellette et al. (2017) and Ouellette et al. (2022) is a dedicated survey of galaxies of all morphological types in the Virgo Cluster (see Fig. 1). SHIVir's original purpose was to examine the impact of a cluster environment on galaxy properties using the nearest cluster in the sky: the Virgo Cluster. We focus on the subset of 44 SHIVir spiral galaxies with Hα RCs from long-slit spectra taken at various observatories (Ouellette et al. 2017). We use the velocity errors as reported in the original data. Distances to the SHIVir galaxies were estimated from SB fluctuations where available (Jerjen et al. 2004;Blakeslee et al. 2009); otherwise, a standard cluster distance of 16.5 Mpc is assumed (Mei et al. 2007). Uncertainties are reported where distance measurements are available; for the cluster distance, a conservative value of 3 Mpc was used.
The SHIVir galaxies are a subset of the full Virgo Cluster Catalog (VCC), which is volume complete in a spatial subset of the Virgo Cluster to an absolute magnitude of M B ≤ −13, along with several fainter galaxies to ensure a broad morphology coverage (Binggeli et al. 1985;McDonald et al. 2011). The cross-referencing of all galaxies from the seven surveys above with NED 2 yielded 4208 galaxies with names, coordinates, and redshift. Most galaxies had morphological information, as presented in Fig. 1 where T-type 12 indicates no available data (3.3% of the PROBES sample). Objects were matched by name and confirmed using redshift information in NED and velocity information from the observed RC. In some instances, only RA and DEC coordinates were usable; naming conventions for some older surveys are no longer recognized. Again these were confirmed using redshift information (which is available for all PROBES galaxies). If neither a name nor coordinates could be confidently confirmed, the galaxy was discarded from the survey; this yielded a total sample of 3293 galaxies.

NED Information and Quality Criteria
Furthermore, many galaxies were duplicated between surveys. In such instances, we stacked their RCs as described in Sec. 2.4. A label, called "RC survey", in the main table indicates that multiple surveys contributed to the final RC. The exception is the Mathewson et al. (1992) and Mathewson & Ford (1996) samples for which the Mathewson & Ford (1996) RCs supersede the other; most of the repeated galaxies between the two surveys are indeed from the same observations. Thus we are left with a PROBES sample of 3163 unique galaxies with RCs and matched NED metadata.

Distances
The PROBES compendium distances come from a number of sources including Hubble flow, surface brightness fluctuations, and tip of the red giant branch. For Hubble flow distances, we have used the CosmicFlows-3 calculator from Kourkchi et al. (2020) 3 . Beyond 200 Mpc, we have assumed a Hubble-Lemaître constant of H 0 = 73 km s −1 Mpc −1 (Riess et al. 2021). Heliocentric redshifts were taken from NED and corrected to cosmic microwave background (CMB) redshifts using a standard Fixsen et al. (1996) apex velocity.

Rotation Curves
The PROBES compendium RCs come mainly from Hα long-slit (major axis) spectra, though a few HI RCs were also available. RC measurements are obtained from an observed wavelength, λ o (e.g. from a long slit spectrograph), and converted to a relative velocity, v, using the formula: where λ s is the source wavelength. In the local universe, where PROBES RCs are measured, this approximation is accurate enough for most purposes. At cosmological distances, the recession velocity is a poorly defined quantity since the observed wavelength shift is caused by a combination of relativistic Doppler shift and stretching of spacetime. In such instances, the well defined quantity redshift, z, can then be better related to velocities for the construction of an RC (Bunn & Hogg 2009). In the PROBES regime, the contribution due to stretching of spacetime can simply be treated as a component of the systemic velocity. Fig. 2 shows the spatial extent distribution of RCs that have corresponding photometry. The brown distribution normalizes R last in kpc; normalizations by effective radius, R e , and isophotal radius, R 23.5 , are also presented. The median extent of the PROBES galaxies is 2R e or 1R 23.5 . This contrasts with previous IFU surveys such as CALIFA (Sánchez et al. 2016) and MaNGA (Bundy et al. 2015) which extend to R 23.5 and 1.5R e , respectively. With such deep measurements, the extended PROBES RCs can efficiently probe the flatter region of a galaxy disk beyond the transition from baryon-to dark matter-dominated systems. Our RCs were all fitted with a tanh model and the multiparameter model of C97. The tanh model matches the simple rise and flattening idealization of each RC. The second, C97 multiparameter model, here referred to as the "C97 model", provides a more complete model of the rich variety of RC shapes (Oman et al. 2015;Frosst et al. 2022). Further details about these fits are given in Sec. 3.2.2. Fig. 3 shows median RC shapes in the PROBES compilation in bins of stellar mass (columns) or concentration (rows). Each RC is linearly interpolated to a standard set of radii, and the median is taken for all galaxies which have measurements at those radii. For this figure, stacked RCs were truncated if less than 3 measured profiles contributed to the median profile. The profile radii and velocities were normalized by R 23.5 and V 23.5 , respectively (see Sec. 3). This enables comparisons on the basis of changing shapes alone. Each panel corresponds to a range of concentration and stellar mass values (see Sec. 3) and a clear trend in RC shape can be seen. For higher stellar mass (concentration) at a given concentration (stellar mass), the RC rises faster near the center (Rubin et al. 1985;Madore & Woods 1987;Persic et al. 1996;Sofue & Rubin 2001). In all but the lowest stellar mass bin, the RCs flatten at or before approximately R 23.5 ; indeed, Fig. 2 shows that the majority of PROBES RCs extend to the flattened region. Fig. 4 gives example PROBES RCs for galaxies with a range of stellar masses. As in Fig. 3, a range of RC shapes can be seen from fast rising to very gradual when normalized by R 23.5 . The highest stellar mass example, NGC7753, shows a velocity peak at about 0.2R 23.5 . The PROBES RCs are densely sampled in most cases allowing for more advanced kinematic analysis. In all cases the C97 model fits and the tanh fits agree well within the bounds of the data, though each yield slightly different extrapolations at large radii. Velocity bumps and wiggles, indicative of noncircular motions and other complex kinematic structure, especially near the galaxy center, are not modelled by the C97 or tanh models.

DESI Legacy Imaging Survey Photometry
The DESI Legacy Imaging Survey provides g, r, z photometry for a large 14, 000 deg 2 area of the sky (Dey et al. 2019). With some of the PROBES galaxies lying outside the DESI-LIS footprint, we have constructed a "PROBES photometry" sample of 1677 galaxies for which matching DESI-LIS photometry can be extracted. The automated nonparametric surface photometry package AutoProf (Stone et al. 2021b) was then applied to all available DESI-LIS r-band images, achieving SB thresholds of ∼28 r-mag arcsec −2 (see Fig. 5, all photometry uses the AB magnitude system). AutoProf performs nonparametric isophotal ellipse fitting by minimizing the power in the second Fourier mode along each ellipse as a function of PA and ellipticity. Azimuthally averaged profiles as well as cardinal wedges (along the four major/minor axes from the center of the galaxy) were extracted for all PROBES photometric galaxies. These wedges offer rich information about the symmetry of galaxies and detailed nonaxisymmetric structure, where present. A unique PSF is determined for each observation, however DESI-LIS images typically have a FWHM resolution of ∼1 arcsec.
The fitted isophotal solution for the r-band image of a galaxy serves as a reference for the matching g and z band images for the same galaxy. The "forced photometry" procedure with AutoProf ensures that all the flux values are calculated along the same isophotes for a given galaxy, a requirement for meaningful colour (and therefore stellar mass) measurements. The AutoProf isophotal fitting is entirely automated though it can fail under certain conditions (e.g. overlapping systems, see Stone et al. 2021b). These conditions are flagged by Au-toProf (also automatically); all flags are reported in the main PROBES table (see Sec. 4).
To characterize the depth of the DESI-LIS/AutoProf photometry, we present in Fig. 5   small errors. These data are thus deep enough for a broad suite of structural analyses. Note that the feature seen in the z-band subplot of Fig. 5 with high brightness and high error is caused by bright galaxies which saturate the detectors. Saturated pixels register in AutoProf as high errors at the transition from saturation to real measurements. This feature is also seen, though to a lesser degree, in the g and r bands.

unWISE Photometry
The unWISE survey provides all-sky W1 and W2 band photometry at a resolution of ∼6 arcsec; fluxes are converted to the AB magnitude system for homogeneity. The mid-infrared photometry available through the un-WISE survey is sensitive to older, mass dominant, stellar populations resulting in robust stellar mass measurements (Conroy 2013;Courteau et al. 2014). Most PROBES galaxies are close enough that they can be resolved by unWISE photometry. We have thus performed forced photometry (again using the r-band isophotal solutions as reference) to obtain SB profiles for the entire PROBES photometry sample. Given the low resolution of the unWISE data, this addition mostly benefits total luminosity measurements, allowing for more robust modelling of the SED (the same will be true for GALEX data; see Sec. 2.7). Other structural parameters computed at large radii are also minimally affected by the low resolution.
As for our DESI-LIS data, Fig. 5 shows the depth of all extracted unWISE SB profiles. The unWISE SB profiles are shallower than the matching DESI-LIS profiles, however they exhibit the same general trend with somewhat higher errors before rising quickly at a limiting SB level of ∼27 r-mag arcsec −2 . The W1 and W2 bands extend deep enough for robust measurements of total light, however the low spatial resolution limits the use of structural metrics at low radii.
We forgo the addition of NIR (JHK) bands as currently available surveys lack the desired depth (Skrutskie et al. 2006) or sky coverage (Lawrence et al. 2007).  The GALEX survey provides nearly all-sky FUV and NUV (FUV and NUV, respectively) broadband photometry at a resolution of approximately 4.3 and 5.3 arcsec, respectively; this photometry is also converted to the AB magnitude system for homogeneity. Most PROBES galaxies are close and bright enough for GALEX forced photometry using AutoProf. As with the g, z, W1, and W2 bands, the r-band isophotal solutions were applied via forced photometry to the GALEX FUV and NUV images for uniform colours. Fig. 5 shows the GALEX SB measurement quality. Similar to the unWISE data, the low GALEX resolution thwarts meaningful measure-ments of structural parameters in the UV; especially near the center of each galaxy. However, GALEX data provide useful SED constraints through bands especially sensitive to dust and recent star formation.

STRUCTURAL PARAMETERS
In addition to the suite of RCs and SB profiles, the PROBES compendium offers a comprehensive array of galaxy structural parameters. These include multiple definitions of size, luminosity, velocity, surface density, stellar mass, concentration, and so on.
This section presents a description of the PROBES parameters, how they are calculated and corrected. Our tables include standard parameters evaluated at common radii (R e , R 23.5 , R 1 , etc.) in the r−band.

Corrections
Before we proceed, a discussion of the corrections to photometric and kinematic measurements is warranted. These corrections are applied to the RCs and SB profiles before computing any parameters. Note that the PROBES database of RCs and SB profiles is presented uncorrected (raw), the only exception being the RC data that are presented with the systemic velocity, V sys , removed (Sec. 3.2.2). The following discussion details how the corrections for our structural parameters were computed.

Velocity Corrections
Observed radial velocities, V o (R), are deprojected and corrected for redshift broadening according to: where V c (R) is the corrected line-of-sight velocity, V sys is the fitted systemic (central) velocity from the C97 model (see Sec. 3.2.2), z helio is the heliocentric redshift of the galaxy, and i last is the nominal inclination of the galaxy disk (the inclination of the outermost isophote). The values for the systemic velocities were determined from the fitted RC model. Literature values for the heliocentric velocity of a galaxy are not used for V sys in order to avoid wavelength calibration differences.

Surface Brightness Profile Truncation
To avoid aberrant isophotes from contaminating parameter estimations, SB profiles are truncated if the galaxy is no longer the dominant light source. Isophotes with an uncertainty exceeding 0.3 mag arcsec −2 for g, r, z, W1, W2 bands, or 0.5 mag arcsec −2 for FUV, NUV bands, are first removed from the profile. As seen in Fig. 5, errors rise quickly beyond ∼0.2 mag arcsec −2 . We Figure 5. Comparison of SB errors for the multiband GALEX, DESI-LIS, and unWISE photometry as a function of SB depth. Scatter points were taken from every profile in the PROBES photometry sample, while contours were used in high density regions. Most SB profiles reach at least 26 mag arcsec −2 before errors start rising; some profiles reach 30 mag arcsec −2 with small errors. This deep multiband photometry critically maximizes the scientific potential of the PROBES photometric dataset.
adopt a conservative 0.3 mag arcsec −2 threshold for our truncation level. The SB errors are statistical in nature and do not account for spurious factors such as nearby objects, bright stars, and galactic cirri which can cause systematic fluctuations that are unrepresentative of the galaxy disk. To handle these cases, we fit an exponential disk + floor model to the r-band SB profile outskirts 4 . The "floor" model is also an exponential with a shallow slope to represent the sky background plus interlopers around the galaxy. Once fit, we truncate at the intersection between the exponential disk model and the floor value. Points are reintroduced if they align closely (±1 mag arcsec −2 ) with the inner exponential fit. This truncation radius in the r-band is then applied to all other bands. Fig. 6 shows an example of a truncation which prevents spurious background data from entering further calculations. Fig. 7 shows the truncation results for each band, as well as the relative flux characteristics between different bands. FUV and NUV have by far the lowest signalto-noise, and low flux near the galaxy center which can be caused by heavy dust extinction and/or reduced star formation in the galaxy center. DESI-LIS g, r, z bands have the largest dynamic range and resolution. The rband isophotal solution is also our reference point for the 4 The outskirts are initially defined as the point beyond which the SB profile is a factor of 100 (5 mag arcsec −2 ) dimmer than the central region. This is intended to avoid bright extended bulges and other nonexponential central features.  imaging of all the other bands. The W1, W2 bands have the lowest resolution, as can be seen by the absence of structure in the central regions of ESO 143-G028 (compared to g, r, z bands), though the signal-to-noise for these observations is high enough for reliable global measurements at large radii. Before computing structural parameters, the truncated PROBES photometry (see Sec. 3.1.2) was corrected for Galactic extinction, K correction, and cosmological dimming. The form of the global photometric correction is given as:

Photometric Corrections
where A c is the corrected brightness value, A o is the observed value, A g is the Galactic extinction, A K is the K correction, and A z is a cosmological dimming factor. We do not add any uncertainty to our model from these corrections, though there is certainly a systematic uncertainty introduced with them. We take Galactic extinctions for the DESI-LIS g, r, and z bands from Schlafly & Finkbeiner (2011); for the GALEX FUV and NUV bands, we use E(B − V ) values from Burstein & Heiles (1982) and transformations from Peek & Schiminovich (2013); for unWISE W1 and W2 fluxes, we assume no extinction and therefore apply no correction. K corrections were applied to FUV, NUV, g, r, and z bands using the calculator of Chilingarian & Zolotukhin (2012) 5 ; for W1, W2 bands we use the corrections from Jarrett et al. (2017). K corrections for the PROBES sample are small given the low redshift of the sample, typically less than 0.1 mag for FUV, NUV, g, r, z bands and less than 0.5 mag for W1, W2 bands. Our cosmological dimming correction 5 See http://kcor.sai.msu.ru/ takes the form: where z helio is the heliocentric redshift. The SB scales as (1 + z helio ) 3 for the measurement of specific intensities (flux per Hz per steradian; e.g. in the AB magnitude system), in contrast with (1 + z helio ) 4 for bolometric fluxes (Tolman 1930;Stabenau et al. 2008;Whitney et al. 2020). This correction is small for the relatively nearby PROBES galaxies, typically ranging from 0.005 − 0.05 mag over the range of our data.

Photometry Inclination Correction
Our inclination correction follows a similar procedure to Stone et al. (2021a) which corrects parameters to faceon equivalent, however with a slight variation. In Stone et al. (2021a), the procedure to correct structural parameters was applied after they were extracted; here, we first correct SB profiles (individual isophotes) at all radii before computing structural parameters. Therefore, all derived quantities are assumed inclination corrected as a consequence. The functional form of the inclination correction to surface brightnesses is: where µ c λ is the corrected surface brightness, λ is the band being corrected, µ λ is the observed surface brightness, i last is the disk inclination taken at the last isophote in the r-band profile, and γ λ is the correction coefficient. The last isophote is used to determine the inclination as this most directly samples the disk, which gives a nominal representation of disk inclination and avoids other features such as bars and bulges. Auto-Prof only fits ellipticity and PA above a S/N threshold (S/N per pixel > 3 on average); beyond that point, Au-toProf fixes these values and our inclinations are effectively measured at ∼ 25.5 ± 1.0 mag arcsec −2 in the rband. Since we use forced photometry from the r-band to all others, the inclination is the same regardless of band.
To determine the correction coefficients, we have performed least squares fits between − log 10 (cos(i)) and the λ − W 1 colour for all SB profile measurements in the PROBES dataset. We use the W1-band as our reference point since it is minimally affected by dust and has higher S/N than the W2-band. Since W1 is assumed stable with inclination, we can use any dependence on λ − W 1 colour to correct λ. SBs fainter than 26 mag arcsec −2 , and inclinations greater than 80 deg, were not included in the calculation of corrections. Note that we only directly correct the SB profiles, curves of growth are recomputed by integrating the corrected SB profile. Fig. 8 shows the fitted inclination correction schemes against the raw PROBES surface brightnesses. As expected, the redder bands are found to require less correction. As a check, the same procedure applied to W 1 − W 2 colours gives essentially no correction (just like the z-band). This straightforward correction scheme is adequate for the general data release of the PROBES compendium; more sophisticated prescriptions are beyond the scope of this paper.

Available Parameters
We provide a vast array of structural parameters for the PROBES photometric sample, covering a wide range of radii for all galaxies. A selection of parameters, evaluated at R 23.5 , are presented in Fig. 9 showing the scope of scaling relations available with the data at almost any desired radius.

Radii
It is useful to evaluate a number of fiducial apparent radii for the measurement of other structural parameters. We have adopted the r-band SB profiles to calculate our fiducial radii, as these profiles have high signal-to-noise, good spatial resolution, and low dust extinction. It is also for these reasons that our photometry uses r-band profiles for forced photometry at other bands. For isophotal radii, values from R 22 to R 26 in increments of 0.5 mag arcsec −2 are obtained as shown on Fig. 10. Sampling brighter than 22 mag arcsec −2 would eliminate many galaxies, and reaching fainter than 26 mag arcsec −2 might expose interlopers. Light percentage radii are also computed from 20 % up to 80 % in increments of 10 %, the most common of these being the effective radius R 50 = R e . We also compute stellar mass percentage radii, though they are not shown in Fig. 10 since they are similar to light percentage radii; stellar mass percentage radii are better matched for comparisons with simulations. Stellar surface density radii at 500, 100, 50, 10, 5, 1 M pc −2 also provide useful physical reference points in each galaxy. R last , the radius of the last point in a galaxy's RC is also provided. Ignoring integration times and instrument sensitivities, R last can roughly be viewed as a tracer of the Hα endpoint in a galaxy. Whenever possible, parameters such as luminosity and stellar mass are also computed to infinity by extrapolating the outer SB profile as an exponential disk (see Sec. 3.2.3).

Velocity
Velocities are a critical and integral part of the PROBES compendium and we have extracted represen-tative velocities at all fiducial radii discussed in Sec. 3.2.1 using the tanh and C97 RC models (Sec. 2.4).
The C97 model captures the RC shapes well enough that reliable extrapolations can be performed for most of the PROBES sample. As such, velocities are provided for all fiducial radii (Sec. 3.2.1) even if this involves an extrapolation of the RC. It is straightforward for users to select interpolation measurements only, as desired. The two RC parameterizations have the form: where r is the radial location in the RC, V sys is the systemic velocity of the galaxy, V max is the maximum velocity 6 , r 0 is the center point offset, r t is the turnover radius from the rising to the flat regime, β controls rising/falling strength of the RC outskirts, and γ determines the shape of the RC turnover to "flat." Fig. 11 shows the C97 model residuals for all of the PROBES photometry sample. The radii are normalized by R 23.5 to ensure that like regions between galaxies are being compared. A number of interesting trends stand out in this figure. The top figure shows that typical velocity residuals are within 15 km s −1 . The bottom figure makes clear that this offset cannot be explained solely by statistical errors since the typical errors exceed 1σ. One must invoke noncircular motions, PSF smoothing, and other complex behaviours that are captured in the PROBES RCs. A notable drop in residuals beyond ∼ R 23.5 is partly due to the decline in the number of galaxies with extended RCs beyond that point and to HI RCs being smoother than Hα. Most extended RCs that sample beyond R 23.5 come from the SPARC survey (see Sec. 2.1.6) which uses HI as a velocity tracer.
The absolute velocity residuals ( Fig. 11 upper panel) are more or less constant within R 23.5 , though the contours show that most velocity measurements occur prior to R 23.5 . The relative velocity residuals (Fig. 11 lower panel) increase considerably towards the center, in the central regions (within R 23.5 ) ∆V /σ v ≈ 2.5 when in principle it should be 1. This is expected with the central regions being more dominated by noncircular motions or other complex behaviours which are not modelled or accounted for in the error values. The large relative central errors may also be caused by PSF blur which can affect velocity measurements especially at the center. The outer regions (beyond R 23.5 ) do have ∆V /σ v ≈ 1 as expected for well behaved large disks. For individual cases, it is likely that noncircular motions exist at large radii as well (Spekkens & Sellwood 2007;Widrow et al. 2014;Nandakumar et al. 2022); however, they are not apparent in aggregate.
We also performed the same residual analysis using tanh model fits instead of the C97 model. The resulting distributions were nearly identical, though the average normalized residual in the central regions was ≈ 3.7 (instead of 2.5) owing to the lower expressive power of tanh models to fit more complex features present in the PROBES RCs (e.g. rising/falling outer profiles or bulge feature).

Luminosity
The apparent magnitude, absolute magnitude, and luminosity corresponding to each radius specified in Sec. 3.2.1 are computed in all FUV, NUV, g, r, z, W1, W2 bands. These are computed directly from the Au-toProf curve of growth.
Using a linear interpolation of the curve of growth, the apparent magnitude is computed and then transformed into the absolute magnitude and luminosity according to: M λ = m λ − 5 log 10 (D/10) (8) where M λ is the absolute magnitude in the λ band, m λ is the apparent magnitude, D is the distance in parsecs, L λ is the luminosity, and M ,λ is the corresponding magnitude of the sun. We take our M values from Willmer (2018) for the FUV, NUV, g, r, z, W1, W2 bands, giving 17. 30, 10.16, 5.05, 4.61, 4.50, 5.92, and 6.58 respectively.
The extrapolation to infinity involves fitting an exponential disk through all SB points beyond R 60 , the radius which encloses 60% of all the detected light. The contribution of the exponential disk beyond the last point in the SB profile is added to the total magnitude and further calculations are performed accordingly. The choice of R 60 as the reference point comes from manual experimentation, though other choices do not alter the resulting total magnitudes appreciably (see Section 4.3 of Courteau 1996).

Colours
Colours are a useful tracer of stellar populations in a given galaxy (Conroy 2013;Courteau et al. 2014). These may be evaluated at or within a given radius, and both modes are included in our tables. Colours within a given radius are determined by taking a difference in apparent magnitudes interpolated from a curve of growth, whereas colours at a given radius are determined by taking the difference in SB values.

Concentration
Concentration is a useful morphological metric for the quantitative comparison of the structure of light profiles (Conselice 2014). Various definitions of concentration exist, for a nonparametric concentration we use the following definition: which measures the ratio of the radii enclosing 80 and 20 percent of the total light of a galaxy. As a nonparametric measure, C 28 is universally applicable since it applies to any light profile.
The PROBES compendium tables also include the Sérsic index (Sérsic 1968) as a parametric concentration parameter. The form of the Sérsic function for fitting galaxy light profiles is given below, where I(R) is the intensity as a function of projected radius, R, I e is the intensity at the effective radius, b n is a normalization constant, R e is the effective projected radius, and n is the Sérsic index. Because of the straightforward interpretation of its model parameters, the Sérsic function has been widely used. However, the reliable reproduction of Sérsic parameters between studies can be especially challenging (Arora et al. 2021;Sonnenfeld 2022 Figure 10. Example r-band SB profile for ESO143-G028 with various radial metrics indicated with arrows. For instance, isophotal radii correspond to SB levels ranging from 22 to 26 mag arcsec −2 in steps of 0.5 mag arcsec −2 ; see text for details. These radii are evaluated for all galaxies in the PROBES photometry sample, most other structural parameters are evaluated at all of these radii. Errors on the SB profiles are not shown as they are too small. Surface brightness (SB), in units of mag arcsec −2 in any given photometric band, is a distance-independent quantity (for noncosmological applications) that informs us about the density of galactic systems. A common measure of galaxy brightness is the central SB, which simply takes the SB at R = 0 from a SB profile. The latter is however especially sensitive to seeing variations between observatory sites, between observations at the same site, and dust extinction for bluer bands. The mean SB, Σ in (< R), measured within various characteristic radii, which can extend beyond a few seeing lengths, is more robust to seeing fluctuations. It is defined as: Σ in (< R) = m(R) + 2.5 log 10 (πqR 2 ), where m(R) is the apparent magnitude within a galactocentric radius R and q is the axis ratio.
One may also calculate the SB at a given radius. The local SB at each radius is computed via interpolation of the SB profile. Note that we still report these values for isophotal radii despite their definition being connected to SB values. Our isophotal radii are determined in the r-band and will typically have different SB values in other photometric bands; i.e., the r-band R 25 will not have an SB of 25 mag arcsec −2 in the g-band.

Stellar Mass
The inferred stellar mass within a given radius, or M * (R), is one of the most fundamental galaxy structural parameters as it enables a direct comparison with the- oretical predictions. Unfortunately, stellar masses also carry a large uncertainty in light of the many assumptions that their computation entails (Courteau et al. 2014). Most photometry-based assessments of stellar mass rely on broadband colour transformations, which themselves make assumptions about the stellar populations makeup of a galaxy. The PROBES photometry sample relies on five broadband fluxes in order to constrain the distribution of stellar populations by mass in galaxies 7 . We have used the colour-mass-to-light transformations of Cluver et al. (2014) and Roediger & Courteau (2015) to infer stellar mass estimates. For each stellar mass estimate, a colour and a luminosity are needed from a given band. Our final value of M * (R) is the average of the four resulting stellar mass estimates from the following colour combinations: (g-z, g); (g-r, r); (r-z, z); and (W1-W2, W1). The standard deviation of this estimate gives the reported error.
In general, systematic errors on stellar mass estimates exceed the random errors (Roediger & Courteau 2015); by reporting the scatter in the M * estimates from four band combinations, we present a hybrid of random and systematic errors.

Stellar Surface Density
The combination of Secs. 3.2.6 and 3.2.7 enables us to compute a stellar surface density, Σ * , in units of M pc −2 .
As stellar mass should be band independent, we averaged multiple bands for the computation of Σ * following the same procedure as Sec. 3.2.7.
Stellar surface density profiles allow one to evaluate radii at which certain densities are reached (e.g. Trujillo et al. 2020). Such radii are included in our table of structural parameters for reference (Sec. 4).

Dynamical Mass
Required for studies of the dark matter distribution and gravitation potentials in galaxies, the dynamical mass gives an estimate of the total enclosed mass (baryons+dark matter) of a galaxy (Courteau et al. 2014). A significant product of the PROBES sample is indeed the deep long slit RCs available for every galaxy. These give reliable estimates, within ∼10 % (Binney & Tremaine 2008, Sec. 2.6, Fig. 2.17) of the total enclosed mass within a galactocentric radius R. Here we opt for a straightforward mass calculation using a spherical mass distribution: where M dyn (R) is the estimate of dynamical mass enclosed within radius R, V (R) is the circular velocity at radius R, and G is the gravitational constant. This mass estimate differs slightly for nonspherical mass distributions (Binney & Tremaine 2008), however it is suitable for most applications and does not require specifying an arbitrary or ill-defined mass distribution.

Parameter Uncertainties
All structural parameters have an associated standard error. This is computed by propagating uncertainty from measurement errors using the standard first-order method unless otherwise specified, where σ f is the error on some parameter with functional form f , and p is a parameter which is used in the calculation of f . These errors do not include covariances between other parameters, as such they are not suitable for certain Bayesian error propagations.

DATA TABLES
The raw PROBES data are composed primarily of RCs and SB profiles. The RCs are formatted as shown in Table 1 in a csv file. These data are presented mostly as in the original survey, except with some concessions for homogenization. Velocities are left uncorrected for inclination and redshift. In all cases the systemic velocity of the galaxy has been removed and the RCs have been recentered (see Sec. 3.2.2). All profiles have been flipped such that the approaching side has positive radius values and the receding side has negative radius values. In cases where multiple observations exist, all available RCs were stacked after centering. No averaging was performed, the final combined profile for a given galaxy simply includes all data points from all available profiles for that galaxy. In some cases, RC uncertainties were not provided and we used as a proxy the standard deviation of the residuals to a C97 model fit; these errors per point typically range from 5 − 15 km s −1 . Using the standard deviation of the residuals typically gives conservatives errors by assuming all deviations from the model are due to measurement errors when in fact some may be due to noncircular motions.
The SB profiles are formatted as shown in Table 2 following the format in Stone et al. (2021b). These profiles are outputted by AutoProf; fitting is performed on the r-band profiles and forced photometry, which ensures that colours can be evaluated on the same pixels, is applied for the other bands. For the fitting procedure, we ran the standard AutoProf pipeline and also extracted (wedge) radial profiles. AutoProf performed a number of checks to ensure that most fits converged to reasonable solutions. In some cases, we used fixed centers and/or masks to improve the fits. Still, a fraction of galaxies, 15.7 %, failed at least one check. These failures may result from slight asymmetries, oversaturated pixels, or nearby bright sources. Typically, if only a single flag is raised then the photometry is still adequate for most purposes. Only 2.5 % of galaxies have two or more Au-toProf flags; for most analyses, these galaxies should be discarded. They are however kept in the sample as users may wish specifically to look at these systems for their complexity. However, in such cases the users should manually examine the photometry and consider using the (wedge) radial profiles along the major/minor axes instead of the full ellipse solution. Along with the raw PROBES data (RCs and SB profiles), three tables are provided with information about the PROBES galaxies. The "main table.csv" file includes basic data about all PROBES compendium galaxies: position (RA,DEC), redshift, distance, and photometry information. The latter indicates whether galaxies have photometry and if they were flagged by AutoProf processing.
The "structural parameters.csv" file includes the bulk of the structural parameters information for the PROBES photometry sample. The number of available parameters is very large and cannot easily be recounted here. A consistent formatting scheme is meant to offer an unambiguous interpretation of each column. A given parameter is divided into two parts by a "|" symbol with the left side indicating the parameter being computed and the right side indicating the radial location of that measurement (or any other necessary information about computing that parameter). For example, the column "Col in:g:r|Ri23.5:r" represents the integrated g − r colour within the isophotal radius R 23.5 measured in the r-band. Fig. 12 shows a typical spectral energy distribution constructed from the structural parameters table. Absolute magnitudes were taken from columns "absMag:λ|Ri26:r" where λ is the filter; these were converted to flux units for the figure.
Further, "Mstar|Rp80:r" represents the stellar mass enclosed within the 80% total light radius as determined from the r band profile. This formatting convention is held for all parameters. When stellar mass is used instead of a wavelength band, the "*" character takes its place. Finally, the "model fits.csv" file gives the parameters for standard fitted models. The fitting parameters for the tanh and C97 models applied to the rotation curves are reported here, along with Sérsic fits to each band-specific SB profile. We have presented the PROBES compilation of deep RCs for 3163 galaxies and matching multiband photometry for 1677 of them. An overview of the data characteristics and the convenient formatting for general use was also discussed. The raw data, as well as a large number of homogeneously determined structural parameters, are available for download within the supplementary material.
By linking deep kinematics and photometry for a statistically significant sample, PROBES offers a comprehensive picture of late-type galaxy structure. Updates to the PROBES data base are anticipated as new data become available. For instance, Frosst et al (PROBES-II, in preparation) will emphasize low mass dwarf systems with the addition of 716 nearby galaxies with highquality rotation curves and 578 matching surface photometry profiles derived from DESI-LIS photometry.
We are grateful to the Natural Sciences and Engineering Research Council of Canada, the Ontario Government, and Queen's University for support through various scholarships and grants. Special thanks go to Arjun Dey and John Moustakas for discussions about the DESI Legacy Imaging Survey. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
Software: astropy (Astropy Collaboration et al.  · · · Ellipticity of isophote (= 1 − b/a, where b = isophote semi-minor axis length) ellip e · · · Uncertainty in ellipticity estimate determined by local variability pa deg Position angle of isophote relative to positive y-axis (increasing counter-clockwise) on the image pa e deg Uncertainty in PA estimate determined by local variability pixels count Number of unmasked pixels sampled along isophote or within band maskedpixels count Number of masked pixels rejected along isophote or within band totmag direct mag Total magnitude enclosed in current isophote by direct pixel flux summation