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 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 1992PASP..104..514B, Cacciari et al.
1987A&AS...69..135C 1987A&AS...69..135C, Skillen et al. 1993SAAOC..15...90S 1993SAAOC..15...90S, Liu & Janes
1989ApJS...69..593L 1989ApJS...69..593L, Paczynski 1965AcA....15..115P 1965AcA....15..115P, Jones et al.
1992ApJ...386..646J 1992ApJ...386..646J, Warren 1966MNSSA..25..103W 1966MNSSA..25..103W, Fernley et al.
1989MNRAS.236..447F 1989MNRAS.236..447F, Fernley et al. 1990MNRAS.242..685F 1990MNRAS.242..685F, and
Clementini et al. 2000AJ....120.2054C 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 1989ApJS...69..593L, Barnes et al.
1992PASP..104..514B 1992PASP..104..514B, and Fernley et al. 1993A&AS...97..815F 1993A&AS...97..815F, Skillen
et al. 1989MNRAS.241..281S 1989MNRAS.241..281S, Fernley et al. 1990MNRAS.242..685F 1990MNRAS.242..685F,
Fernley et al. 1989MNRAS.236..447F 1989MNRAS.236..447F and Skillen et al.
1993MNRAS.265..301S 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 2010AJ....140.1868W; see
also Cutri et al. 2012, Cat. II/311) or NEOWISE (Mainzer et al.
2011ApJ...731...53M 2011ApJ...731...53M, Mainzer et al. 2014, Cat. J/ApJ/792/30)
photometry is available for each of our stars.
File Summary:
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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
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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)
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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 1998MNRAS.293L..61F);
d = Clementini et al. (2000AJ....120.2054C 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 1990ApJ...354..273L;
2 = Jones et al. 1992ApJ...386..646J 1992ApJ...386..646J;
3 = Skillen et al. 1993MNRAS.265..301S 1993MNRAS.265..301S;
4 = Fernley et al. 1989MNRAS.236..447F 1989MNRAS.236..447F;
5 = Jones et al. 1988ApJ...332..206J 1988ApJ...332..206J;
6 = Cacciari et al. 1989A&A...209..154C 1989A&A...209..154C;
7 = Fernley et al. 1990MNRAS.242..685F 1990MNRAS.242..685F;
8 = Skillen et al. 1989MNRAS.241..281S 1989MNRAS.241..281S.
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Byte-by-byte Description of file: table3.dat
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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)
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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 1993MNRAS.265..301S);
5 = Barnes et al. (1992PASP..104..514B 1992PASP..104..514B);
7 = Liu & Janes (1989ApJS...69..593L 1989ApJS...69..593L);
8 = Liu & Janes (1990ApJ...354..273L 1990ApJ...354..273L);
9 = Barcza & Benko (2014MNRAS.442.1863B 2014MNRAS.442.1863B);
10 = Paczynski (1965AcA....15..115P 1965AcA....15..115P);
11 = 2MASS (Cutri et al. 2003, Cat. II/246);
17 = ASAS Pojmanski (1997AcA....47..467P 1997AcA....47..467P);
15 = Jones et al. (1992ApJ...386..646J 1992ApJ...386..646J);
19 = IBVS Broglia & Conconi (1992IBVS.3748....1B 1992IBVS.3748....1B);
31 = Fernley et al. (1990MNRAS.242..685F 1990MNRAS.242..685F);
41 = Fernley et al. (1989MNRAS.236..447F 1989MNRAS.236..447F);
98 = Clementini et al. (1990A&AS...85..865C 1990A&AS...85..865C);
99 = Clementini et al. (2000AJ....120.2054C 2000AJ....120.2054C);
999 = Three-hundred MilliMeter Telescope (TMMT), modified for Blazhko
effect.
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Byte-by-byte Description of file: table4.dat
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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)
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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).
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Byte-by-byte Description of file: table5.dat
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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)
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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.
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Byte-by-byte Description of file: table6.dat
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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
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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.
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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].
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History:
From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 28-Jun-2017