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- ID:
- ivo://CDS.VizieR/J/A+A/559/A35
- Title:
- FBS 0117+396 pulsating sdB star photometry
- Short Name:
- J/A+A/559/A35
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims to discover subdwarf-B stars with massive compact companions such as overmassive white dwarfs (M>1.0M_{sun}_), neutron stars or black holes. From the 127 subdwarfs with substantial radial-velocity variations discovered in the initial survey, a number of interesting objects have been selected for extensive follow-up. After an initial photometry run with BUSCA revealed that FBS0117+396 is photometrically variable both on long and short timescales, we chose it as an auxiliary target during a 6-night multi-color photometry run with Ultracam. Spectroscopy was obtained at a number of observatories in order to determine the binary period and obtain a radial-velocity amplitude. After establishing an orbital period of P=0.252d, and removing the signal associated with the irradiated hemisphere of the M-dwarf companion, we were able to detect ten pulsation periods in the Fourier spectrum of the light curve. Two pulsation modes are found to have short periods of 337 and 379s, and at least eight modes are found with periods between 45-min and 2.5h. This establishes that FBS0117+396 is an sdB+dM reflection binary, in which the primary is a hybrid pulsator, and the first one found with this particular melange of flavours.
- ID:
- ivo://CDS.VizieR/J/AJ/152/158
- Title:
- Final Kepler transiting planet search (DR25)
- Short Name:
- J/AJ/152/158
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present results of the final Kepler Data Processing Pipeline search for transiting planet signals in the full 17-quarter primary mission data set. The search includes a total of 198709 stellar targets, of which 112046 were observed in all 17 quarters and 86663 in fewer than 17 quarters. We report on 17230 targets for which at least one transit signature is identified that meets the specified detection criteria: periodicity, minimum of three observed transit events, detection statistic (i.e., signal-to-noise ratio) in excess of the search threshold, and passing grade on three statistical transit consistency tests. Light curves for which a transit signal is identified are iteratively searched for additional signatures after a limb-darkened transiting planet model is fitted to the data and transit events are removed. The search for additional planets adds 16802 transit signals for a total of 34032; this far exceeds the number of transit signatures identified in prior pipeline runs. There was a strategic emphasis on completeness over reliability for the final Kepler transit search. A comparison of the transit signals against a set of 3402 well-established, high-quality Kepler Objects of Interest yields a recovery rate of 99.8%. The high recovery rate must be weighed against a large number of false-alarm detections. We examine characteristics of the planet population implied by the transiting planet model fits with an emphasis on detections that would represent small planets orbiting in the habitable zone of their host stars.
- ID:
- ivo://CDS.VizieR/VI/44
- Title:
- Finding List of Interacting Binaries, 5th ed.
- Short Name:
- VI/44
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This catalog is abstracted from the Card Catalog maintained at the University of Florida containing information on all published, and to the extent available, unpublished work on eclipsing binaries. The fifth edition differs from the previous ones in the extension of the magnitude limit at maximum light from 13 to 15. The catalog fields are Finding List number; star name; position (equinox 1900); blue magnitude at maximum light; bandpass of maximum light; depth of primary minimum in same bandpass; bandpass primary minimum; depth of secondary minimum and its bandpass; spectral class of star eclipsed at primary light and optional uncertainty character; spectral class of star eclipsed at secondary light; most recent reliable epoch of primary minimum; most recent orbital period; duration of primary minimum; duration of totality of primary minimum; BD, CoD, CPD, and HD number; alternate designations of system; codes indicating the nature of the system.
- ID:
- ivo://CDS.VizieR/J/AJ/159/187
- Title:
- First RVs with the EXPRES spectrograph: 51Peg
- Short Name:
- J/AJ/159/187
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The EXtreme-PREcision Spectrograph (EXPRES) is an environmentally stabilized, fiber-fed, R=137500, optical spectrograph. It was recently commissioned at the 4.3m Lowell Discovery Telescope near Flagstaff, Arizona. The spectrograph was designed with a target radial-velocity (RV) precision of 30cm/s. In addition to instrumental innovations, the EXPRES pipeline, presented here, is the first on-sky, optical, fiber-fed spectrograph to employ many novel techniques-including an "extended flat" fiber used for wavelength-dependent quantum efficiency characterization of the CCD, a flat-relative optimal extraction algorithm, chromatic barycentric corrections, chromatic calibration offsets, and an ultra-precise laser frequency comb for wavelength calibration. We describe the reduction, calibration, and RV analysis pipeline used for EXPRES and present an example of our current sub-meter-per-second RV measurement precision, which reaches a formal, single-measurement error of 0.3m/s for an observation with a per-pixel signal-to-noise ratio of 250. These velocities yield an orbital solution on the known exoplanet host 51Peg that matches literature values with a residual rms of 0.895m/s.
- ID:
- ivo://CDS.VizieR/J/A+A/624/A118
- Title:
- Fitted orbits and parameters of 51 Eridani b
- Short Name:
- J/A+A/624/A118
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- 51 Eridani observations were performed with the VLT exoplanet imager SPHERE for 3 years in order to monitor the orbital motion of the known giant planet and refine its orbital parameters. We carried out an orbital analysis using three complementary approaches (LSMC, MCMC, Bayesian rejection sampling) and found broadly similar results. The data suggest a period of 23-49yr (i.e. semi-major axis of 10-16au), an inclination of 126-147{deg}, an eccentricity of 0.30-0.55, and an argument at periastron of 57-121{deg} (mod 180{deg}). The time at periastron and the longitude of node exhibit bimodal distributions.
- ID:
- ivo://CDS.VizieR/J/AJ/158/63
- Title:
- Five new transiting hot Jupiters:HATS-54b-HATS-58b
- Short Name:
- J/AJ/158/63
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery by the HATSouth project of five new transiting hot Jupiters (HATS-54b through HATS-58Ab). HATS-54b, HATS-55b, and HATS-58Ab are prototypical short-period (P=2.5-4.2 days, R_p_~1.1-1.2 R_J_) hot Jupiters that span effective temperatures from 1350 to 1750 K, putting them in the proposed region of maximum radius inflation efficiency. The HATS-58 system is composed of two stars, HATS-58A and HATS-58B, which are detected thanks to Gaia DR2 data and which we account for in the joint modeling of the available data-with this, we are led to conclude that the hot Jupiter orbits the brighter HATS-58A star. HATS-57b is a short-period (2.35 day), massive (3.15 M_J_), 1.14 R_J_, dense (2.65+/-0.21 g/cm^3^) hot Jupiter orbiting a very active star (2% peak-to-peak flux variability). Finally, HATS-56b is a short-period (4.32 day), highly inflated hot Jupiter (1.7 R_J_, 0.6 M_J_), which is an excellent target for future atmospheric follow-up, especially considering the relatively bright nature (V=11.6) of its F dwarf host star. This latter exoplanet has another very interesting feature: the radial velocities show a significant quadratic trend. If we interpret this quadratic trend as arising from the pull of an additional planet in the system, we obtain a period of P_c_=815_-143_^+253^ days for the possible planet HATS-56c, and a minimum mass of M_c_sini_c_=5.11+/-0.94 M_J_. The candidate planet HATS-56c would have a zero-albedo equilibrium temperature of T_eq_=332+/-50 K, and thus would be orbiting close to the habitable zone of HATS-56. Further radial-velocity follow-up, especially over the next two years, is needed to confirm the nature of HATS-56c.
- ID:
- ivo://CDS.VizieR/J/AJ/145/68
- Title:
- Five new transit light curves of TrES-3
- Short Name:
- J/AJ/145/68
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Five newly observed transit light curves of the TrES-3 planetary system are presented. Together with other light-curve data from the literature, 23 transit light curves in total, which cover an overall timescale of 911 epochs, have been analyzed through a standard procedure. From these observational data, the system's orbital parameters are determined and possible transit timing variations (TTVs) are investigated. Given that a null TTV produces a fit with reduced {chi}^2^=1.52, our results agree with previous work, that TTVs might not exist in these data. However, a one-frequency oscillating TTV model, giving a fit with a reduced {chi}^2^=0.93, does possess a statistically higher probability. It is thus concluded that future observations and dynamical simulations for this planetary system will be very important.
- ID:
- ivo://CDS.VizieR/J/A+A/591/A55
- Title:
- Five transiting hot Jupiters discovered using WASP
- Short Name:
- J/A+A/591/A55
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have used photometry from the WASP-South instrument to identify 5 stars showing planet-like transits in their light curves. The planetary nature of the companions to these stars has been confirmed using photometry from the EulerCam instrument on the Swiss Euler 1.2-m telescope and the TRAPPIST telescope, and spectroscopy obtained with the CORALIE spectrograph. The planets discovered are hot Jupiter systems with orbital periods in the range 2.17 to 5.75 days, masses from 0.3M_{Jup}_ to 1.2M_{Jup}_ and with radii from 1R_{Jup}_ to 1.5R_{Jup}_. These planets orbit bright stars (V=11-13) with spectral types in the range F9 to G4. WASP-126 is the brightest planetary system in this sample and hosts a low-mass planet with a large radius (0.3M_{Jup}_, 0.95R_{Jup}_), making it a good target for transmission spectroscopy. The high density of WASP-129 A suggests that it is a helium-rich star similar to HAT-P-11 A. WASP-133 has an enhanced surface lithium abundance compared to other old G-type stars, particularly other planet host stars. These planetary systems are good targets for follow-up observations with ground-based and space-based facilities to study their atmospheric and dynamical properties.
- ID:
- ivo://CDS.VizieR/J/MNRAS/368/1392
- Title:
- Flares of the close binary FL Vir
- Short Name:
- J/MNRAS/368/1392
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The results of U-filter flare monitoring of the binary flare star FL Vir = Wolf 424 is presented. 57 flares with energies between 2x10^28^ and 2x10^31^erg were recorded in 20h of observation. The properties of flare occurrence and flare time-scales are analysed, and the flare activity level in 1980 April is determined to be L_f_(U)=8.0x10^26^erg/s. This is larger than previously published results and may indicate a variation in the flare activity level on a time-scale of years. An analysis of existing data indicates that the flare activity level correlates with the relative orbital positions of the stars.
