- ID:
- ivo://CDS.VizieR/J/ApJ/622/217
- Title:
- Light and motion in the local volume
- Short Name:
- J/ApJ/622/217
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using high-quality data on 149 galaxies within 10Mpc, I find no correlation between luminosity and peculiar velocity at all. There is no unequivocal sign on scales of 12Mpc of the expected gravitational effect of the brightest galaxies, in particular infall toward groups, or of infall toward the supergalactic plane on any scale. Either dark matter is not distributed in the same way as luminous matter in this region, or peculiar velocities are not due to fluctuations in mass. The sensitivity of peculiar velocity studies to the background model is highlighted.
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Search Results
- ID:
- ivo://CDS.VizieR/J/AJ/137/507
- Title:
- Light and velocity curves of VZ Cep
- Short Name:
- J/AJ/137/507
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present new V-band differential photometry and radial velocity measurements of the unevolved, 1.18 day period, F+G-type, double-lined eclipsing binary VZ Cep. We determine accurate values for the absolute masses, radii, and effective temperatures.
- ID:
- ivo://CDS.VizieR/J/ApJ/838/122
- Title:
- Light curve analysis of 13 active stars
- Short Name:
- J/ApJ/838/122
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present results from light curve fits to the photometry of 13 chromospherically active stars, covering the time evolution of the rotational phase of their primary light curve minimum and the light curve amplitude.
- ID:
- ivo://CDS.VizieR/J/AJ/162/7
- Title:
- Light curve and radial velocities for 7 host stars
- Short Name:
- J/AJ/162/7
- Date:
- 18 Mar 2022 09:35:03
- Publisher:
- CDS
- Description:
- We report the discovery and characterization of seven transiting exoplanets from the HATNet survey. The planets, which are hot Jupiters and Saturns transiting bright Sun-like stars, include: HAT-P-58b (with mass M_p_=0.37M_J_, radius R_p_=1.33R_J_, and orbital period P=4.0138days), HAT-P-59b (M_p_=1.54M_J_, R_p_=1.12R_J_, P=4.1420days), HAT-P-60b (M_p_=0.57M_J_, R_p_=1.63R_J_, P=4.7948days), HAT-P-61b (M_p_=1.06M_J_, R_p_=0.90R_J_, P=1.9023days), HAT-P-62b (M_p_=0.76M_J_, R_p_=1.07R_J_, P=2.6453days), HAT-P-63b (M_p_=0.61M_J_, R_p_=1.12R_J_, P=3.3777days), and HAT-P-64b (M_p_=0.58M_J_, R_p_= 1.70R_J_, P=4.0072days). The typical errors on these quantities are 0.06M_J_, 0.03R_J_, and 0.2s, respectively. We also provide accurate stellar parameters for each of the host stars. With V=9.710{+/-}0.050mag, HAT-P-60 is an especially bright transiting planet host, and an excellent target for additional follow-up observations. With R_p_=1.703{+/-}0.070R_J_, HAT-P-64b is a highly inflated hot Jupiter around a star nearing the end of its main-sequence lifetime, and is among the largest known planets. Five of the seven systems have long-cadence observations by TESS which are included in the analysis. Of particular note is HAT-P-59 (TOI-1826.01) which is within the northern continuous viewing zone of the TESS mission, and HAT-P-60, which is the TESS candidate TOI-1580.01.
- ID:
- ivo://CDS.VizieR/J/AJ/133/255
- Title:
- Light-curve and radial velocities of BD+42 2782
- Short Name:
- J/AJ/133/255
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- BD+42 2782 was recently discovered to be a variable star with a W UMa-type, eclipsing-binary light curve. We have obtained the first photoelectric light curves (R_C_, I_C_) and also the first radial velocity curves for this binary.
- ID:
- ivo://CDS.VizieR/J/ApJ/654/L25
- Title:
- Light-curve data for GRB 050319
- Short Name:
- J/ApJ/654/L25
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Multiwavelength observations of the optical afterglow of GRB 050319 were performed from 1.31 to 9.92hr after the burst. Our R-band light curves, combined with other published data, can be described by the smooth broken power-law function, with {alpha}_1_=-0.84+/-0.02 to {alpha}_2_=-0.48+/-0.03, 0.04 days after the gamma-ray burst. The optical light curves are characterized by shallow decays as was also observed in the X-rays which may have a similar origin, related to energy injection. However, our observations indicate that there is still a puzzle concerning the chromatic breaks in the R-band light curve (at 0.04 days) and the X-ray light curve (at 0.004 days) that remains to be solved.
- ID:
- ivo://CDS.VizieR/J/ApJ/641/L13
- Title:
- Light-curve data for GRB 030329
- Short Name:
- J/ApJ/641/L13
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present multicolor optical observations of the nearby (z=0.1685) gamma-ray burst GRB 030329 obtained with the same instrumentation over a time period of 6 hours, for a total of an unprecedented 475 quasi-simultaneous BVR observations.
- ID:
- ivo://CDS.VizieR/J/A+A/649/A98
- Title:
- Lightcurve inversion for 491 asteroids
- Short Name:
- J/A+A/649/A98
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- We perform lightcurve inversion for 491 asteroids to retrieve phase curve parameters, rotation periods, pole longitudes and latitudes, and convex and triaxial ellipsoid shapes by using the sparse photometric observations from Gaia Data Release 2 and the dense ground-based observations from the DAMIT data base. We develop a method for the derivation of reference absolute magnitudes and phase curves from the Gaia data, allowing for comparative studies among hundreds of asteroids.
- ID:
- ivo://CDS.VizieR/J/A+A/625/A152
- Title:
- Light-curve models of black hole
- Short Name:
- J/A+A/625/A152
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In the new era of gravitational wave (GW) and multi-messenger astrophysics, the detection of a GW signal from the coalescence of a black hole - neutron star (BHNS) binary remains a highly anticipated discovery. This kind of system is expected to be within reach of the second generation of ground-based detectors. In this context, we develop a series of versatile semi-analytical models to predict the properties of all the electromagnetic (EM) counterparts of BHNS mergers.We include the nuclear-decay-powered kilonova emission, its radio remnant, the prompt emission from the jet and the related afterglow. The properties of these counterparts depend upon those of the outflows that result from the partial disruption of the NS during the merger and from the accretion disc around the remnant, which are necessary ingredients for transient EM emission to accompany the GW signal. We therefore define ways to relate the properties of these outflows to those of the progenitor binary, establishing a link between the binary parameters and the counterpart properties. From the resulting model, we anticipate the variety of light curves that can emerge after a BHNS coalescence, from the radio up to gamma-rays. These light curves feature universal traits which are the imprint of the dynamics of the emitting outflows, but at the same time they show a clear dependence on the BH mass and spin, though with a high degree of degeneracy. The latter can be deduced by joint GW - EM analysis. In this paper, we perform a proof-of-concept multi-messenger parameter estimation of a BHNS merger with an associated kilonova, to test how the information from the EM counterpart can complement that from the GW signal. Our results indicate that the observation and modeling of the kilonova can help to break the degeneracies in the GW parameter space, leading to better constraints on, e.g., the BH spin.
- ID:
- ivo://CDS.VizieR/J/A+A/576/A18
- Title:
- Light curve of (2060) Chiron
- Short Name:
- J/A+A/576/A18
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We propose that several short-duration events observed in past stellar occultations by Chiron were produced by ring material. Some similarities between these events and the characteristics of Chariklo's rings could indicate common mechanisms around centaurs. From a reanalysis of the stellar occultation data in the literature, we determined two possible orientations of the pole of Chiron's rings, with ecliptic coordinates {lambda}=(352+/-10){deg}, {beta}=(37+/-10){deg} or {lambda}=(144+/-10){deg}, {beta}=(24+/-10){deg}. The mean radius of the rings is (324+/-10)km. One can use the rotational lightcurve amplitude of Chiron at different epochs to distinguish between the two solutions for the pole. Both solutions imply a lower lightcurve amplitude in 2013 than in 1988, when the rotational lightcurve was first determined. We derived Chiron's rotational lightcurve in 2013 from observations at the 1.23m CAHA telescope, and indeed its amplitude was smaller than in 1988. We also present a rotational lightcurve in 2000 from images taken at the CASLEO 2.15m telescope that is consistent with our predictions. Out of the two poles, the {lambda}=(144+/-10){deg}, {beta}=(24+/-10){deg} solution provides a better match to a compilation of rotational lightcurve amplitudes from the literature and those presented here. We also show that using this preferred pole orientation, Chiron's long-term brightness variations are compatible with a simple model that incorporates the changing brightness of the rings while the tilt angle with respect to the Earth is changing with time. Also, the variability of the water ice band in Chiron's spectra as seen in the literature can be explained to a large degree by an icy ring system whose tilt angle changes with time and whose composition includes water ice, analogously to the case of Chariklo. We present several possible formation scenarios for the rings from qualitative points of view and speculate on why rings might be common in centaurs. We also speculate on whether the known bimodal color distribution of the centaurs could be due to centaurs with rings and centaurs without rings.
