- ID:
- ivo://CDS.VizieR/J/A+A/450/1149
- Title:
- Radial velocity curve of Balloon 090100001
- Short Name:
- J/A+A/450/1149
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have obtained 2552 useful low-resolution spectra of the bright sdBV Balloon 090100001, which form the first large time-resolved spectroscopic dataset of this brightest known pulsating subdwarf B star. The data were obtained at the Nordic Optical Telescope during 7 nights in August/September 2004 over a total time base of 38 nights, aiming to derive pulsational characteristics of this star. In this paper we present the observations and the results obtained from frequency analyses. In our data we find clear evidence for 8 independent frequencies, that were all previously reported in photometric monitoring studies, allowing future asteroseismological studies of this star to be constrained by combined photometric and spectroscopic observations of as much as 8 pulsation modes. We do not find conclusive evidence for new frequencies. We present the first determination of the pulsational radial-velocity amplitudes of this star, and find that the radial-velocity amplitude of the main pulsation mode (f_1_=2.80749mHz) in Balloon 090100001 is 18.9km/s, which is the largest radial-velocity amplitude found in sdB-star pulsations so far.
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- ID:
- ivo://CDS.VizieR/J/AJ/148/114
- Title:
- Radial velocity curve of {delta} Cir
- Short Name:
- J/AJ/148/114
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Delta Cir is known as an O7.5 III eclipsing and spectroscopic binary with an eccentric orbit. Penny et al. discovered the presence of a third component in the IUE spectra. The eclipsing binary and the third body revolve around a common center of gravity with a period of 1644days in an eccentric orbit with a semimajor axis of 10AU. We demonstrate the presence of apsidal-line rotation with a period of {approx}141yr, which is considerably longer than its theoretically predicted value, based on the published radii of the binary components derived from the Hipparchos H_p_ light curve. However, our new solution of the same light curve resulted in smaller radii and better agreement between the observed and predicted period of the apsidal-line advance. There are indications that the third body is a binary. The object was resolved by VLTI using the PIONIER combiner; in 2012 June, the separation was 3.78mas with magnitude difference in the H region 1.75fm. This result means that (assuming a distance of 770pc) the inclination of the long orbit is 87.7{deg}.
- ID:
- ivo://CDS.VizieR/J/A+A/509/A24
- Title:
- Radial velocity curve of {gamma}^1^ Leo
- Short Name:
- J/A+A/509/A24
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Our primary goal is to search for planets around intermediate mass stars. We are also interested in studying the nature of radial velocity (RV) variations of K giant stars. We selected about 55 early K giant (K0-K4) stars brighter than fifth magnitude that were observed using BOES, a high resolution spectrograph attached to the 1.8m telescope at BOAO (Bohyunsan Optical Astronomy Observatory). BOES is equipped with I_2_ absorption cell for high precision RV measurements. We detected a periodic radial velocity variations in the K0 III star gamma1 Leo with a period of P=429-days. An orbital fit of the observed RVs yields a period of P=429-days, a semi-amplitude of K=208m/s, and an eccentricity of e=0.14. To investigate the nature of the RV variations, we analyzed the photometric, Ca II {lambda} 8662 equivalent width, and line-bisector variations of gamma1 Leo. We conclude that the detected RV variations can be best explained by a planetary companion with an estimated mass of msini=8.78M_{Jupiter}_ and a semi-major axis of a=1.19AU, assuming a stellar mass of 1.23M_{sun}_.
- ID:
- ivo://CDS.VizieR/J/A+A/469/1069
- Title:
- Radial velocity curve of {gamma} Peg
- Short Name:
- J/A+A/469/1069
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- With this work we provide observational material to study magnetic field variability of the classical beta Cep-type star gamma Peg. The observations were carried out in the HeI 6678 line in the course of 23 observing nights from 1997 to 2005 with using coude spectrograph in spectropolarimetric mode at the Crimean 2.6m telescope. The behavior of stellar wind was studied in the UV region using data from the IUE satellite (the INES database). It is shown that the UV stellar wind exhibits a variability. A variation of the wind due to stellar pulsations has been detected. In the HeI 6678 line the abnormally blueshifted radial velocities (gamma=-60.57+/-0.29km/s) were detected during a single night in 2005. We do not confirm the 370.5-day orbital period. The most probable orbital period was estimated as P_orb_=6.81608+/-0.00012d. The ratio P_orb_/P_puls_=44.92 appeared to be very close to integer. We have detected the presence of weak magnetic field on the star. The longitudinal component of the field varies from -10G to 30G with the stellar rotation. The most probable rotational period is P_rot_=6.6538+/-0.0016d. Both the orbital and the rotational periods are integral multiple of the difference between them: P_orb_/|P_orb_-P_rot_|=42.002, and P_rot_/|P_orb_-P_rot_|=41.002. Variation of the longitudinal magnetic field during pulsation period with an amplitude about 7G has been detected.
- ID:
- ivo://CDS.VizieR/J/A+A/519/A10
- Title:
- Radial velocity curve of HD 202206
- Short Name:
- J/A+A/519/A10
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Long-term, precise Doppler measurements with the CORALIE spectrograph have revealed the presence of two massive companions to the solar-type star HD 202206. Although the three-body fit of the system is unstable, it was shown that a 5:1 mean motion resonance exists close to the best fit, where the system is stable. It was also hinted that stable solutions with a wide range of mutual inclinations and low O-C were possible. We present here an extensive dynamical study of the HD 202206 system, aiming at constraining the inclinations of the two known companions, from which we derive possible value ranges for the companion masses.
- ID:
- ivo://CDS.VizieR/J/A+A/495/959
- Title:
- Radial velocity curve of HD 189733
- Short Name:
- J/A+A/495/959
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Extra-solar planet search programs require high-precision velocity measurements. They need to study how to disentangle radial-velocity variations due to Doppler motion from the noise induced by stellar activity. We monitored the active K2V star HD 189733 and its transiting planetary companion that has a 2.2-day orbital period. We used the high-resolution spectrograph SOPHIE mounted on the 1.93-m telescope at the Observatoire de Haute-Provence to obtain 55 spectra of HD 189733 over nearly two months. We refined the HD 189733b orbit parameters and put limits on the eccentricity and on a long-term velocity gradient. After subtracting the orbital motion of the planet, we compared the variability of spectroscopic activity indices to the evolution of the radial-velocity residuals and the shape of spectral lines. The radial velocity, the spectral-line profile and the activity indices measured in HeI (5875.62{AA}), Halpha (6562.81{AA}) and the CaII H&K lines (3968.47{AA} and 393 3.66{AA}) show a periodicity around the stellar rotation period and the correlations between them are consistent with a spotted stellar surface in rotation. We used such correlations to correct for the radial-velocity jitter due to stellar activity. This results in achieving high precision on the orbit parameters, with a semi-amplitude K=200.56+/-0.88m/s and a derived planet mass of M_P_=1.13+/-0.03M_{Jup}_.
- ID:
- ivo://CDS.VizieR/J/A+A/610/A3
- Title:
- Radial velocity curve of 3 K giants
- Short Name:
- J/A+A/610/A3
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The purpose of this paper is to detect and investigate the nature of long-term radial velocity (RV) variations of K-type giants and to confirm planetary companions around the stars. We have conducted two planet search programs by precise RV measurement using the 1.8m telescope at Bohyunsan Optical Astronomy Observatory (BOAO) and the 1.88m telescope at Okayama Astrophysical Observatory (OAO). The BOAO program searches for planets around 55 early K giants. The OAO program is looking for 190 G-K type giants. In this paper, we report the detection of long-period RV variations of three K giant stars, HD 40956, HD 111591, and HD 113996. We investigated the cause of the observed RV variations and conclude the substellar companions are most likely the cause of the RV variations. The orbital analyses yield P=578.6+/-3.3d, msini=2.7+/-0.6M_J_, a=1.4+/-0.1AU for HD 40956; P=1056.4+/-14.3d, msini=4.4+/-0.4M_J_, a=2.5+/-0.1AU for HD 111591; P=610.2+/-3.8d, msini=6.3+/-1.0M_J_, a=1.6+/-0.1AU for HD 113996.
- ID:
- ivo://CDS.VizieR/J/AJ/153/138
- Title:
- Radial velocity curve of 51 Peg
- Short Name:
- J/AJ/153/138
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the detection of water absorption features in the day side spectrum of the first-known hot Jupiter, 51 Peg b, confirming the star-planet system to be a double-lined spectroscopic binary. We use high-resolution (R{approx}100000), 3.2{mu}m spectra taken with CRIRES/VLT to trace the radial-velocity shift of the water features in the planet's day side atmosphere during 4 hr of its 4.23 day orbit after superior conjunction. We detect the signature of molecular absorption by water at a significance of 5.6{sigma} at a systemic velocity of V_sys_=-33+/-2km/s, coincident with the 51 Peg host star, with a corresponding orbital velocity K_P_=133_-3.5_^+4.3^km/s. This translates directly to a planet mass of M_p_=0.476_-0.031_^+0.032^M_J_, placing it at the transition boundary between Jovian and Neptunian worlds. We determine upper and lower limits on the orbital inclination of the system of 70{deg}<i<82.2{deg}. We also provide an updated orbital solution for 51 Peg b, using an extensive set of 639 stellar radial velocities measured between 1994 and 2013, finding no significant evidence of an eccentric orbit. We find no evidence of significant absorption or emission from other major carbon-bearing molecules of the planet, including methane and carbon dioxide. The atmosphere is non-inverted in the temperature-pressure region probed by these observations. The deepest absorption lines reach an observed relative contrast of 0.9*10^-3^ with respect to the host star continuum flux at an angular separation of 3 milliarcseconds. This work is consistent with a previous tentative report of K-band molecular absorption for 51 Peg b by Brogi et al.
- ID:
- ivo://CDS.VizieR/J/PASP/118/1238
- Title:
- Radial velocity curve of RBS 490
- Short Name:
- J/PASP/118/1238
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- RBS (ROSAT Bright Source) 0490 is a cataclysmic variable star (CV) with unusually strong emission lines. The strength of the emission lines has led to a suggestion that the object is intrinsically faint and correspondingly nearby (33pc), which, if true, would strongly affect estimates of the CV space density. Here we report astrometry, filter photometry, and time-series spectroscopy of this object. The astrometry gives an absolute parallax of 4.5+/-1.5mas and a relative proper motion of 102mas/yr. A Bayesian procedure gives a very uncertain distance estimate of d~300pc, and the small parallax alone implies d>133pc (at 2 standard deviations). The mean V magnitude is 17.4, which implies M_V_=10.9-5log[d/(200pc)], neglecting extinction. At 200pc, the space velocity would be over 90km/s with respect to the local standard of rest. The time-series spectroscopy shows a possible emission-line radial velocity period near 46 minutes. This would be unusually short for an orbital period, and it may represent some other clock in the system.
- ID:
- ivo://CDS.VizieR/J/A+AS/123/209
- Title:
- Radial velocity curve of Sigma Gem
- Short Name:
- J/A+AS/123/209
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The table contains the radial velocities of the RS CVn star sigma Geminorum measured by cross-correlation using Beta Oph as template from the high-resolution SOFIN spectra around 6175A.
