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J/AJ/154/49  Transiting Exoplanet Monitoring Project. II. HAT-P-33 (Wang+, 2017)

Transiting Exoplanet Monitoring Project (TEMP). II. Refined system parameters and Transit Timing analysis of HAT-P-33b. Wang Y.-H., Wang S., Liu H.-G., Hinse T.C., Laughlin G., Wu D.-H., Zhang X., Zhou X., Wu Z., Zhou J.-L., Wittenmyer R.A., Eastman J., Zhang H., Hori Y., Narita N., Chen Y., Ma J., Peng X., Zhang T.-M., Zou H., Nie J.-D., Zhou Z.-M. <Astron. J., 154, 49-49 (2017)> =2017AJ....154...49W (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Photometry, RI Keywords: planetary systems - planets and satellites: fundamental parameters - planets and satellites: individual HAT-P-33b - stars: fundamental parameters - stars: individual: HAT-P-33 - techniques: photometric Abstract: We present 10 R-band photometric observations of eight different transits of the hot Jupiter HAT-P-33b, which has been targeted by our Transiting Exoplanet Monitoring Project. The data were obtained by two telescopes at the Xinglong Station of National Astronomical Observatories of China (NAOC) from 2013 December through 2016 January, and exhibit photometric scatter of 1.6-3.0mmag. After jointly analyzing the previously published photometric data, radial-velocity (RV) measurements, and our new light curves, we revisit the system parameters and orbital ephemeris for the HAT-P-33b system. Our results are consistent with the published values except for the planet to star radius ratio (RP/R*), the ingress/egress duration (τ) and the total duration (T14), which together indicate a slightly shallower and shorter transit shape. Our results are based on more complete light curves, whereas the previously published work had only one complete transit light curve. No significant anomalies in Transit Timing Variations (TTVs) are found, and we place upper mass limits on potential perturbers, largely supplanting the loose constraints provided by the extant RV data. The TTV limits are stronger near mean-motion resonances, especially for the low-order commensurabilities. We can exclude the existence of a perturber with mass larger than 0.6, 0.3, 0.5, 0.5, and 0.3M near the 1:3, 1:2, 2:3, 3:2, and 2:1 resonances, respectively. Description: We have recorded a total of 10 light curves of eight different transits events observed by two telescopes (a 60/90cm Schmidt and a 60cm telescope) at Xinglong Station operated by National Astronomical Observatories of China (NAOC) between 2013 December and 2016 January. Two of the transit events were observed by the two telescopes simultaneously. The first seven transit events were monitored by the 60/90cm Schmidt telescope. It has a 4K*4K CCD with a ∼94'*∼94' field of view, which gives a pixel scale of 1.38''/pixel. The transit events that occurred on UT 2014 February 27 and UT 2014 March 6 were also simultaneously observed by the 60cm, and the last transit in our sequence was also monitored with this telescope. The 60cm telescope is equipped with a 512*512 CCD and covers a field of view of 17'*17', resulting in a pixel scale of 1.95''/pixel. Objects: ----------------------------------------------------------------------- RA (ICRS) DE Designation(s) (Period) ----------------------------------------------------------------------- 07 32 44.22 +33 50 06.1 HAT-P-33 = GSC 02461-00988 (P=3.47447472) ----------------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 81 10 Overview of observations and data reduction table2.dat 38 3732 Photometry of HAT-P-33 table4.dat 40 17 Mid-transit times for HAT-P-33b
See also: J/ApJ/785/126 : HIRES radial velocity measurements (Knutson+, 2014) J/ApJ/742/59 : HAT-P-32 and HAT-P-33 follow-up (Hartman+, 2011) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 11 A11 "Y:M:D" Date UTC date of observation 13- 20 A8 "h:m:s" Time0 Starting UTC time of observation 22- 29 A8 "h:m:s" Time1 Ending UTC time of observation 31- 37 A7 --- Tel Telescope (G1) 39 A1 --- Flt [R] Filter 41- 43 I3 --- Frames Number of frames 45- 46 I2 s Exp1 First exposure time 48- 50 I3 s Exp2 ? Second exposure time 52 I1 s Read Readout time 54- 57 F4.2 --- Airmass1 Airmass 59- 62 F4.2 --- Airmass2 Airmass 64- 67 F4.2 --- Airmass3 ? Airmass 69- 72 F4.2 --- Moon Moon illum. 74 I1 --- Comp Comp. stars 76- 77 I2 pix Aper Aperture diameter around star 79- 81 F3.1 mmag Scatter Root-mean-square (rms) of residual from our best-fitting model
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 14 F14.6 d BJD Date of observation in Barycentric Julian Date (BJD); BJDTDB time standard (1) 16- 21 F6.4 --- RFlux [0.9799/1.0103] Relative flux in Flt 23- 28 F6.4 mag Scatter [0.0016/0.0038] Root-mean-square (rms) of residual from our best-fitting model 30- 36 A7 --- Tel Telescope used in the observation (60cm or Schmidt) (G1) 38 A1 --- Flt [R] Filter used in the observation (R)
Note (1): All the timing throughout the paper are based on BJDTDB, calculated from Coordinated Universal Time (UTC) using the procedure developed by Eastman et al. (2010PASP..122..935E).
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 4 I4 --- E [-557/392] Epoch (1) 6- 12 A7 --- Tel Telescope (FLWO, Schmidt, or 60cm) (G1) 14- 26 F13.5 d BJD Mid-transit time Tc (BJDTDB) 28- 32 F5.2 s e_BJD [31.2/64] Uncertainty of mid-transit time (σTc) 34- 40 F7.2 s O-C [-192.4/211.56] The (O-C) residual
Note (1): The first seven time points are obtained from the published light curves (Hartman et al. 2011, Cat. J/ApJ/742/59) through separate fits, the others are from our photometric data. The epochs (239, 241) were followed by two telescopes simultaneously.
Global Notes: Note (G1): Telescope used in the observation are defined as follows: Schmidt = 60/90cm Schmidt at the Xinglong Station of National Astronomical Observatories of China (NAOC); 60cm = 60cm telescope at the Xinglong Station of NAOC; FLWO = Fred Lawrence Whipple Observatory (FLWO) in Arizona. For more information about the FLWO telescope, see Hartman et al. 2011 (Cat. J/ApJ/742/59).
History: From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 24-Oct-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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