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J/AJ/153/96    Standard Galactic field RR Lyrae. I. Photometry   (Monson+, 2017)

Standard Galactic field RR Lyrae. I. Optical to mid-infrared phased photometry. Monson A.J., Beaton R.L., Scowcroft V., Freedman W.L., Madore B.F., Rich J.A., Seibert M., Kollmeier J.A., Clementini G. <Astron. J., 153, 96-96 (2017)> =2017AJ....153...96M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Stars, bright ; Stars, nearby ; Photometry, UBVRI ; Photometry, infrared ; Abundances, [Fe/H] Keywords: stars: variables: RR Lyrae Abstract: We present a multi-wavelength compilation of new and previously published photometry for 55 Galactic field RR Lyrae variables. Individual studies, spanning a time baseline of up to 30 years, are self-consistently phased to produce light curves in 10 photometric bands covering the wavelength range from 0.4 to 4.5 microns. Data smoothing via the GLOESS technique is described and applied to generate high-fidelity light curves, from which mean magnitudes, amplitudes, rise times, and times of minimum and maximum light are derived. 60000 observations were acquired using the new robotic Three-hundred MilliMeter Telescope (TMMT), which was first deployed at the Carnegie Observatories in Pasadena, CA, and is now permanently installed and operating at Las Campanas Observatory in Chile. We provide a full description of the TMMT hardware, software, and data reduction pipeline. Archival photometry contributed approximately 31000 observations. Photometric data are given in the standard Johnson UBV, Kron-Cousins RCIC, 2MASS JHK, and Spitzer [3.6] and [4.5] bandpasses. Description: The Three-hundred MilliMeter Telescope (TMMT) is a fully robotic, 300mm telescope at Las Campanas Observatory (LCO), for which the nightly operation and data processing have been completely automated. Over the course of two years data were collected on 179 individual nights for our sample of the 55 RR Lyrae in the B, V, and IC broadband filters. Of these nights, 76 were under photometric conditions and calibrated directly. The 103 nonphotometric nights were roughly calibrated by using the default transformation equations, but only provide differential photometry relative to the calibrated frames. This resulted in 59698 final individual observations. Individual data points have a typical photometric precision of 0.02mag. The statistical error falls rapidly with hundreds of observations, with the zero-point uncertainties being the largest source of uncertainty in the final reported mean magnitude. To compare the results of our TMMT campaign to previous studies of these RR Lyrae (RRL) and to fill gaps in our TMMT phase coverage, we have compiled available broadband data from literature published over the past 30 years and spanning our full wavelength coverage (0.4 to 4.5µm) from the optical to mid-infrared. We have homogenized these diverse data sets to the following filter systems: Johnson UBV, Kron-Cousins RI, 2MASS J,H,Ks, and Spitzer [3.6], [4.5]. The All Sky Automated Survey (ASAS; http://www.astrouw.edu.pl/asas/) is a long-term project monitoring all stars brighter than V∼14mag. The program covers both hemispheres, with telescopes at Las Campanas Observatory in Chile and Haleakala on Maui, both of which provide simultaneous I and V photometry. The GEOS RR Lyr Survey (http://www.ast.obs-mip.fr/users/leborgne/dbRR/grrs.html) is a long-term program utilizing TAROT (http://tarot.obs-hp.fr/) at Calern Observatory (Nice University, France). Annual data releases from this project add times for maximum light for program stars over the last year of observations. In addition to the large programs previously described, we use optical data from individual studies over the past 30 years (Barnes et al. 1992PASP..104..514B, Cacciari et al. 1987A&AS...69..135C, Skillen et al. 1993SAAOC..15...90S, Liu & Janes 1989ApJS...69..593L, Paczynski 1965AcA....15..115P, Jones et al. 1992ApJ...386..646J, Warren 1966MNSSA..25..103W, Fernley et al. 1989MNRAS.236..447F, Fernley et al. 1990MNRAS.242..685F, and Clementini et al. 2000AJ....120.2054C). Single-epoch photometry is available from 2MASS (Cutri et al. 2003, Cat. II/246) in J, H, and Ks. Data from Sollima et al. 2008 (Cat. J/MNRAS/384/1583), Liu & Janes 1989ApJS...69..593L, Barnes et al. 1992PASP..104..514B, and Fernley et al. 1993A&AS...97..815F, Skillen et al. 1989MNRAS.241..281S, Fernley et al. 1990MNRAS.242..685F, Fernley et al. 1989MNRAS.236..447F and Skillen et al. 1993MNRAS.265..301S are adopted. The mid-infrared [3.6] and [4.5] observations were taken using Spitzer/IRAC as part of the Warm-Spitzer Exploration Science Carnegie RR Lyrae Program (CRRP; PID 90002, Freedman et al. 2012sptz.prop90002F). WISE (Wright et al. 2010AJ....140.1868W; see also Cutri et al. 2012, Cat. II/311) or NEOWISE (Mainzer et al. 2011ApJ...731...53M, Mainzer et al. 2014, Cat. J/ApJ/792/30) photometry is available for each of our stars. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 78 55 RR Lyrae (RRL) Galactic calibrators and ephemerides table3.dat 54 90243 Three-hundred MilliMeter Telescope (TMMT) photometry and phased archival data table4.dat 27 94208 Gaussian-windowed LOcal regrESSion (GLOESS) light curves table5.dat 139 55 Intensity mean magnitudes from Gaussian-windowed LOcal regrESSion (GLOESS) light curves table6.dat 199 55 Amplitudes, minimum magnitude and rise times from Gaussian-windowed LOcal regrESSion (GLOESS) light curves
See also: I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) J/ApJ/792/30 : NEOWISE magnitudes for near-Earth objects (Mainzer+, 2014) J/AJ/142/187 : HST observations of 7 Pop.II variables (Benedict+, 2011) J/MNRAS/386/2115 : Type II Cepheid and RR Lyrae variables (Feast+, 2008) J/MNRAS/384/1583 : JHK light curves of RR Lyr (Sollima+, 2008) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Name Star name 11- 21 F11.9 d FPer [0.25/0.74] Final period 23- 34 F12.4 d HJD Three-hundred MilliMeter Telescope (TMMT) HJD-max 36- 45 E10.3 d/yr zeta [-0.0015/0.0019]? Quadratic O-C shape term (ζ), if required 47- 50 A4 --- RRL RR Lyrae class (either RRab, RRc, or RRd) 52- 58 F7.2 d BLPer [7.2/1748.9]? Blazhko effect period 60- 64 F5.2 [Sun] [Fe/H] [-2.6/-0.07] Metallicity (1) 66 A1 --- r_[Fe/H] Reference flag on [Fe/H] (2) 68- 70 A3 --- HIP [HIP] Parallax from Hipparcos (HIP) (3) 72- 74 A3 --- BW Parallax from Baade-Wesselink (3) 76- 78 A3 --- HST [HST] Parallax from HST (HST) (3)
Note (1): Unless otherwise noted, values are taken from Feast et al. 2008 (Cat. J/MNRAS/386/2115), but the measurements were first compiled by Fernley et al. 1998 (Cat. J/A+A/330/515) and references therein and are on a metallicity scale defined by Fernley & Barnes 1997 (Cat. J/A+AS/125/313) and references therein. Note (2): Reference codesa are defined as follows: c = Fernley et al. (1998MNRAS.293L..61F); d = Clementini et al. (2000AJ....120.2054C). Note (3): The codes indicating where the parallax is derived from are defined as follows: HIP = Hipparcos (see Cat. I/239); HST = Hubble Space Telescope (see Benedict et al. 2011, Cat. J/AJ/142/187); 1 = Liu & Janes 1990ApJ...354..273L; 2 = Jones et al. 1992ApJ...386..646J; 3 = Skillen et al. 1993MNRAS.265..301S; 4 = Fernley et al. 1989MNRAS.236..447F; 5 = Jones et al. 1988ApJ...332..206J; 6 = Cacciari et al. 1989A&A...209..154C; 7 = Fernley et al. 1990MNRAS.242..685F; 8 = Skillen et al. 1989MNRAS.241..281S.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Name Star name 11- 12 A2 --- Flt Filter (G1) 14- 19 F6.3 mag mag [6.1/20.3] Vega magnitude in Flt 21- 26 F6.3 mag e_mag [0.001/3.9]?=99.005 Uncertainty in mag (σphot) 28- 32 F5.3 mag err [0.003/0.05] Systematic error in the zero-point determination (σsys) 34- 43 F10.4 d MJD Heliocentric Modified Julian Day (HJD-2400000.5) 45- 49 F5.3 deg Phase [0/1] Final derived phase (Φ) 51- 54 I4 --- Ref [0/999]? References (1)
Note (1): Reference codes are defined as follows: 0 = Three-hundred MilliMeter Telescope (TMMT), this work; 1 = Spitzer, this work; 4 = Skillen et al. (1993MNRAS.265..301S); 5 = Barnes et al. (1992PASP..104..514B); 7 = Liu & Janes (1989ApJS...69..593L); 8 = Liu & Janes (1990ApJ...354..273L); 9 = Barcza & Benko (2014MNRAS.442.1863B); 10 = Paczynski (1965AcA....15..115P); 11 = 2MASS (Cutri et al. 2003, Cat. II/246); 17 = ASAS Pojmanski (1997AcA....47..467P); 15 = Jones et al. (1992ApJ...386..646J); 19 = IBVS Broglia & Conconi (1992IBVS.3748....1B); 31 = Fernley et al. (1990MNRAS.242..685F); 41 = Fernley et al. (1989MNRAS.236..447F); 98 = Clementini et al. (1990A&AS...85..865C); 99 = Clementini et al. (2000AJ....120.2054C); 999 = Three-hundred MilliMeter Telescope (TMMT), modified for Blazhko effect.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Name Star name 11- 12 A2 --- Flt Filter (G1) 14- 20 F7.5 deg Phase [0/1] Phase 22- 27 F6.3 mag mag [6.3/14.1] Gaussian-windowed LOcal regrESSion (GLOESS) Vega magnitude (1)
Note (1): Mean magnitudes were determined by computing the mean intensity of the evenly sampled GLOESS fit points to the light curve, then converting back to a magnitude. The light curve must be sampled with enough data points to capture all the nuances of the shape for an accurate mean; in our case we sampled with 256 data points spaced every 1/256 in phase. Generally, GLOESS fits were determined only for those stars and bands that had more than 20 individual data points over a reasonable portion of phase (i.e., 20 data points only spanning Φ∼0.1 would not have a GLOESS fit nor a mean magnitude).
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Name Star name 11- 16 F6.3 mag <Umag> [8/13]? Intensity mean Johnson U band magnitude 18- 22 F5.3 mag e_<Umag> [0.01/0.021]? Uncertainty in Umag (4) 24- 29 F6.3 mag <Bmag> [8/14]? Intensity mean Johnson B band magnitude 31- 35 F5.3 mag e_<Bmag> [0.003/0.021]? Uncertainty in Bmag (4) 37- 42 F6.3 mag <Vmag> [7.7/13.4]? Intensity mean Johnson V band magnitude 44- 48 F5.3 mag e_<Vmag> [0.003/0.021]? Uncertainty in Vmag (4) 50- 55 F6.3 mag <Rmag> [9.2/11.9]? Intensity mean Kron-Cousins RC band magnitude 57- 61 F5.3 mag e_<Rmag> [0.02/0.02]? Uncertainty in Rmag (4) 63- 68 F6.3 mag <Imag> [7.2/12.88]? Intensity mean Kron-Cousins IC band magnitude 70- 74 F5.3 mag e_<Imag> [0.003/0.028]? Uncertainty in Imag (4) 76- 81 F6.3 mag <Jmag> [6.74/11.21]? Intensity mean 2MASS J band magnitude 83- 87 F5.3 mag e_<Jmag> [0.009/0.02]? Uncertainty in Jmag (4) 89- 94 F6.3 mag <Hmag> [6.5/11]? Intensity mean 2MASS H band magnitude 96-100 F5.3 mag e_<Hmag> [0.013/0.013]? Uncertainty in Hmag (4) 102-107 F6.3 mag <Ksmag> [6.49/10.89]? Intensity mean 2MASS Ks band magnitude 109-113 F5.3 mag e_<Ksmag> [0.009/0.009]? Uncertainty in Ksmag (4) 115-120 F6.3 mag <[3.6]> [6.47/12.27]? Intensity mean Spitzer/IRAC 3.6µm band magnitude 122-126 F5.3 mag e_<[3.6]> [0.008/0.011]? Uncertainty in [3.6] (4) 128-133 F6.3 mag <[4.5]> [6.46/12.25]? Intensity mean Spitzer/IRAC 4.5µm band magnitude 135-139 F5.3 mag e_<[4.5]> [0.008/0.011]? Uncertainty in [4.5] (4)
Note (4): The random uncertainty of the Gaussian-windowed LOcal regrESSion (GLOESS)-derived mean magnitude is simply the error on the mean of data points going into GLOESS fitting. Thus, stars with more data points will have a smaller uncertainty in GLOESS mean magnitude. The systematic uncertainty is determined by the photometric transformations, either in transforming our Three-hundred MilliMeter Telescope (TMMT) photometry onto an absolute system (see Figure 2) or as reported in the literature and in transforming from other filter systems (as described in Section 4). The final reported error is: σ2=1/∑(1/σ2phot)+1/∑(1/σ2sys), where the sum over σsys includes only the unique entries from each reference, i.e., it is not counted for every measurement.
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Name Star name 11- 15 F5.3 mag Uamp [0.46/1.74]? Amplitude in Johnson U band (5) 17- 22 F6.3 mag Umin [8.5/13.4]? Minimum U band magnitude at HJDmax 24- 28 F5.3 --- RTU [0.1/0.44]? U band rise time (5) 30- 34 F5.3 mag Bamp [0.46/1.7]? Amplitude in Johnson B band (5) 36- 41 F6.3 mag Bmin [8.5/14.1]? Minimum B band magnitude at HJDmax 43- 47 F5.3 --- RTB [0.1/0.51]? B band rise time (5) 49- 53 F5.3 mag Vamp [0.35/1.31]? Amplitude in Johnson V band (5) 55- 60 F6.3 mag Vmin [8/13.6]? Minimum V band magnitude at HJDmax 62- 66 F5.3 --- RTV [0.1/0.5]? V band rise time (5) 68- 72 F5.3 mag Ramp [0.3/1.1]? Amplitude in Kron-Cousins RC band (5) 74- 79 F6.3 mag Rmin [9.5/12.3]? Minimum RC band magnitude at HJDmax 81- 85 F5.3 --- RTR [0.13/0.45]? RC band rise time (5) 87- 91 F5.3 mag Iamp [0.1/0.9]? Amplitude in Kron-Cousins IC band (5) 93- 98 F6.3 mag Imin [7.5/13.1]? Minimum IC band magnitude at HJDmax 100-104 F5.3 --- RTI [0.1/0.48]? IC band rise time (5) 106-110 F5.3 mag Jamp [0.2/0.6]? Amplitude in 2MASS J band (5) 112-117 F6.3 mag Jmin [6.9/11.5]? Minimum J band magnitude at HJDmax 119-123 F5.3 --- RTJ [0.12/0.5]? J band rise time (5) 125-129 F5.3 mag Hamp [0.23/0.38]? Amplitude in 2MASS H band (5) 131-136 F6.3 mag Hmin [6.7/11.3]? Minimum H band magnitude at HJDmax 138-142 F5.3 --- RTH [0.18/0.52]? H band rise time (5) 144-148 F5.3 mag Ksamp [0.09/0.34]? Amplitude in 2MASS Ks band (5) 150-155 F6.3 mag Ksmin [6.6/11.2]? Minimum Ks band magnitude at HJDmax 157-161 F5.3 --- RTKs [0.19/0.56]? Ks band rise time (5) 163-167 F5.3 mag 3.6amp [0.05/0.35]? Amplitude in Spitzer/IRAC 3.6µm band (5) 169-174 F6.3 mag 3.6min [6.6/12.4]? Minimum IRAC 3.6µm magnitude at HJDmax 176-180 F5.3 --- RT3.6 [0.17/0.6]? IRAC 3.6µm rise time (5) 182-186 F5.3 mag 4.5amp [0.06/0.36]? Amplitude in IRAC 4.5µm band (5) 188-193 F6.3 mag 4.5min [6.6/12.4]? Minimum IRAC 4.5µm band magnitude at HJDmax 195-199 F5.3 --- RT4.5 [0.16/0.93]? IRAC 4.5µm band rise time
Note (5): Amplitude (aλ) and rise time (RTλ) are defined as the difference in magnitude (mag) and phase (dimensionless), respectively, between the minimum and maximum of the Gaussian-windowed LOcal regrESSion (GLOESS) light curve.
Global Notes: Note (G1): Either Johnson U, Johnson B, Johnson V, Kron-Cousins R, Kron-Cousins I, 2MASS J, 2MASS H, 2MASS K, S1=Spitzer/IRAC [3.6], or S2=Spitzer/IRAC [4.5].
History: From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 28-Jun-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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