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Seventeen New Variable Stars Detected in Vulpecula and Perseus

I report the discovery of seventeen new variable stars in the Northern Sky: three eclipsing (GSC 02129-00759; GSC 02129-00947; GSC 02869-02559), one eruptive (GSC 02856-02521), ten pulsating (2MASS J19305329+2558520; GSC 02129- 00537; 2MASS J19323543+2524000; 2MASS J19263580+2616428; HD 275169; GSC 02869-00313; GSC 02869-01981; GSC 02856-01391; GSC 02860-01552; GSC 02856-01465) and three rotating (one of which is suspected) (GSC 02142-01107; GSC 02856-00169; GSC 02865-01593).


Introduction
Starting in the spring of 2011 the Keyhole Observatory MPC K48, located in S. Giorgio di Mantova (Italy), has been involved in an intense surveying activity mainly focused on new variable star discovery and characterization. Even this year a new observing campaign was conducted in three separate fields located in the constellations of Vulpecula and Perseus for a total of 28 nights, obtaining 2,583 images in the V passband with an overall exposure time of almost 86 hours.
Subsequently, the light curves of all stars in the fields in a magnitude range between 9 V and 14 V have been visually inspected in order to determine the candidate variables, starting with those that have an RMS scatter as function of magnitude higher than normal. When possible the observations were combined with SuperWASP (Butters et al. 2010), ASAS-3 (Pojmański 2002), and NSVS (Wożniak et al. 2004) datasets to enhance the precision in the determination of the period, magnitude range, and the type of variability.
Considering all the new variables discovered, two are in my opinion the most interesting: GSC 02856-02521, an RS CVn variable with Algol-type eclipses, and GSC 02860-01552, a high-amplitude d Scuti (HADS) double mode variable.

Instrumentation used
The data were obtained with a TS Optics APO906 Carbon, a triplet FPL-53 apochromatic refractor with 90-mm aperture and f/6.6 focal ratio; the telescope was also equipped with a field flattener for pin-point stellar images corner-to-corner.
The telescope was positioned at coordinates 45° 12' 33" N, 10° 50' 20" E (WGS84) at the Keyhole Observatory, a rolloff roof structure managed by the author. The pointing was maintained with a Syntha NEQ6 mount guided via a Baader Vario Finder telescope equipped with a Barlow lens capable of bringing the focal length of the system to 636 mm and focal ratio of f/10.5. The guide camera was a Magzero MZ-5 with Micron MT9M001 monochrome sensor. The CCD camera was a SBIG ST8300m with monochrome sensor Kodak KAF8300. The photometry in the Johnson V passband was performed with an Astrodon Photometrics Johnson-V 50-mm round unmounted filter, equipping a Starlight Xpress USB filterwheel.
The camera is equipped with a 1,000× antiblooming: after exhaustive testing it has been verified that the zone of linear response is between 1,000 and 20,000 ADU, although up to 60,000 ADU the loss of linearity is less than 5%. The CCD is equipped with a single-stage Peltier cell ΔT = 35 ± 0.1° C which allows the cooling at a stationary temperature.
These fields were chosen to maximize the possibility of discovering new variable stars. Their determination was made trying to meet the following criteria: • equatorial coordinates compatible with low air masses for most of the night at the observing site; • low or no presence of already known variables, where this element has been determined by analyzing the distribution of the variables in the International Variable Star Index operated by the AAVSO (VSX; Watson et al. 2014).
The observations were performed with the CCD at a temperature of -10° C (in summer and fall) and -20° C (in winter) in binning 1 × 1. The exposure time was 120 seconds with a delay of 1 second between the images and an average download time of 11 seconds per frame. Once the images were obtained, a full calibration procedure was performed with dark and flat frames. All images were then aligned and an astrometric reduction made to implement the astrometrical WCS coordinate system in the FITS header. All these operations were conducted entirely through the use of software maximdl V5.23 (Diffraction Limited 2012). The complete observing log is reported in Table 1.

Methods and procedures
As a continuation of the wider survey activity conducted from the Keyhole Observatory MPC K48 for new variable star discovery, the methods and procedures used will be presented in a very schematic way; in previously published works (Furgoni 2013a(Furgoni , 2013b) more specific details can be found.
The technique used for the determination of the magnitude was differential photometry, ensemble-type in almost all cases. It is necessary to have comparison stars with magnitudes accurately determined in order to obtain reliable measurements and as close as possible to the standard system. Since the entire observational campaign was conducted with the use of the Johnson V filter the comparison star magnitudes were obtained from the APASS (Henden et al. 2013) V magnitude data provided by the AAVSO.
The search for new variable stars was performed using the same technique described in Furgoni (2013aFurgoni ( , 2013b: the method involves the distinction between discovery nights and follow-up nights. The first is needed to determine if the chosen field contains potential candidate variables through the creation of a magnitude-RMS diagram and the accurate visual inspection of all light curves down to the fourteenth magnitude. If in the discovery night the chosen field does not appear interesting it is discarded without further analysis. The follow-up nights, instead, are necessary for the collection of data concerning variable star candidates. In any case, any follow-up night is checked again by a magnitude-RMS scatter diagram. In this case, however, the light curves of the stars in the field are not inspected visually due to the long time needed for the operation. The combination of these two ways of working ensures a good compromise between the need to maximize the chance of discovery and to obtain the maximum from the data gradually collected. Before proceeding further in the analysis, the time of the light curves obtained was heliocentrically corrected (HJD) in order to ensure a perfect compatibility of the data with observations carried out even at a considerable distance in time. When necessary, the determination of the period was calculated using the software period04 (Lenz and Breger 2005), using a Discrete Fourier Transform (DFT). The average zeropoint (average magnitude of the object) was subtracted from the dataset to prevent the appearance of artifacts centered at frequency 0.0 of the periodogram. The calculation of the uncertainties was carried out with period04 using the method described in Breger et al. (1999).
To improve the period determination, SWASP, ASAS-3, and NSVS photometric data were used when available. However, due to the high scattering which in some cases affects both, the data with high uncertainties were eliminated. The datasets were also corrected in their zero-point to make them compatible with my V band data. Having the same zero-point is indeed crucial for correct calculation of the Discrete Fourier Transform operated by period04.

New variable stars discovered
In this survey seventeen new variable stars were discovered belonging to a population composed as follows: • Three eclipsing (two b Lyrae and one b Persei).
• Ten pulsating (six Delta Scuti, one double-mode High Amplitude Delta Scuti, one RR Lyrae Ab-type , one RR Lyrae C-type and one Semi-Regular late-type).
• Three rotating (three rotating ellipsoidal, one of which is suspected).
The coordinates of all new variable stars discovered in this survey are reported as they appear in the UCAC4 catalogue (Zacharias et al. 2012) and never differ from the detected positions for a value greater than 1".                       Wise et al. (1993). Possibile presence of a secondary period. Phase plot is shown in Figure  13; light curve is shown in Figure 14.   (7) Epoch: 2457064.3295(9) HJD Ensemble Comparison Stars: UCAC4 666-016582 (APASS 11.679 V); UCAC4 666-016538 (APASS 11.519 V) Check Star: UCAC4 666-016446 Notes: J-K = 0.23; SWASP magnitudes contaminated by UCAC4 666-016412 (V = 11.500; sep. 24"). SWASP range has been corrected. Phase plot is shown in Figure 15.        Schlafly and Finkbeiner (2011). Phase plot is shown in Figure 19.   Schlafly and Finkbeiner (2011). There is a 17.0 V mag. star 7" to the SSE. The magnitudes are for the blend of both stars. If the identification is correct and the variable is not the fainter star (unlikely), the deblended range would be V = 13.86-13.97.

Ephemeris from Furgoni dataset
Considering that the calculated epoch and period of almost all the variable stars discovered in this campaign are obtained from a combination of my observations and those from other surveys like ASAS, SWASP, and NSVS, it is necessary to point out that this way of work does not necessarily give precise period calculation. In effect almost all the periods are very short, and there are long lasting gaps between my observations and those in the other campaigns or databases. Therefore, in some cases there could be ambiguities in determining the accurate number of cycles that had passed during these gaps. Because of that I want to give for all the short period stars combined with other datasets an additional ephemeris calculated only with my dataset. However, for the stars listed in sections 5.8 and 5.12 I don't provide my own ephemeris because without the other survey datasets it is impossible to make a reasonable period calculation. In addition, for some stars where the cycle count problem is more relevant (sections 5.3, 5.4, 5.7, and 5.9) the period calculation was made weighting the data in relation to the uncertainty: with this approach I try to minimize the effect of most scattered data in the DFT calculation and provide a better period and error calculation. The results are presented in Table 3.

Dedication and acknowledgements
I want to dedicate this work to my loved cat Tillo, who passed away this summer, after many years as an irreplaceable companion under the starry sky.