- ID:
- ivo://CDS.VizieR/J/AJ/156/140
- Title:
- Four new eclipsing mid M-dwarf systems from MEarth
- Short Name:
- J/AJ/156/140
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using data from the MEarth-North and MEarth-South transit surveys, we present the detection of eclipses in four mid M-dwarf systems: LP 107-25, LP 261-75, LP 796-24, and LP 991-15. Combining the MEarth photometry with spectroscopic follow-up observations, we show that LP 107-25 and LP 796-24 are short-period (1.388 and 0.523 day, respectively) eclipsing binaries in triple-lined systems with substantial third-light contamination from distant companions. LP 261-75 is a short-period (1.882 day) single-lined system consisting of a mid M-dwarf eclipsed by a probable brown dwarf secondary, with another distant visual brown dwarf companion. LP 991-15 is a long-period (29.3 day) double-lined eclipsing binary on an eccentric orbit with a geometry that produces only primary eclipses. A spectroscopic orbit is given for LP 991-15, and initial orbits for LP 107-25 and LP 261-75.
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- ID:
- ivo://CDS.VizieR/J/A+A/510/A100
- Title:
- Four new SDSS eclipsing systems
- Short Name:
- J/A+A/510/A100
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present photometry of nine cataclysmic variable stars identified by the Sloan Digital Sky Survey, aimed at measuring the orbital periods of these systems. Four of these objects show deep eclipses, from which we measure their orbital periods. The light curves of three of the eclipsing systems are also analysed using the LCURVE code, and their mass ratios and orbital inclinations determined. SDSS J075059.97+141150.1 has an orbital period of 134.1564+/-0.0008min, making it a useful object with which to investigate the evolutionary processes of cataclysmic variables. SDSS J092444.48+080150.9 has a period of 131.2432+/-0.0014min and is probably magnetic. The white dwarf ingress and egress phases are very deep and short, and there is no clear evidence that this object has an accretion disc. SDSS J115207.00+404947.8 and SDSS J152419.33+220920.1 are nearly identical twins, with periods of 97.5+/-0.4 and 93.6+/-0.5min and mass ratios of 0.14+/-0.03 and 0.17+/-0.03, respectively. Their eclipses have well-defined white dwarf and bright spot ingress and egress features, making them excellent candidates for detailed study. All four of the orbital periods presented here are shorter than the 2-3 hour period gap observed in the known population of cataclysmic variables.
- ID:
- ivo://CDS.VizieR/J/ApJ/830/51
- Title:
- FourStar galaxy evolution survey (ZFOURGE)
- Short Name:
- J/ApJ/830/51
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The FourStar galaxy evolution survey (ZFOURGE) is a 45 night legacy program with the FourStar near-infrared camera on Magellan and one of the most sensitive surveys to date. ZFOURGE covers a total of 400arcmin^2^ in cosmic fields CDFS, COSMOS and UDS, overlapping the CANDELS fields.
- ID:
- ivo://CDS.VizieR/J/MNRAS/420/2580
- Title:
- Four transits of HAT-P-13
- Short Name:
- J/MNRAS/420/2580
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present photometry of four transits of the planetary system HAT-P-13, obtained using defocused telescopes. We analyse these, plus nine data sets from the literature, in order to determine the physical properties of the system. The mass and radius of the star are M_A_=1.320+/-0.048+/-0.039M_{sun}} and R_A_=1.756+/-0.043+/-0.017R_{sun}_ (statistical and systematic error bars). We find the equivalent quantities for the transiting planet to be M_b_=0.906+/-0.024+/-0.018M_Jup_ and R_b_=1.487+/-0.038+/-0.015R_Jup_, with an equilibrium temperature of T'_eq_=1725+/-31K. Compared to previous results, which were based on much sparser photometric data, we find the star to be more massive and evolved, and the planet to be larger, hotter and more rarefied.
- ID:
- ivo://CDS.VizieR/J/ApJ/652/1715
- Title:
- Four transits of the exoplanet XO-1b
- Short Name:
- J/ApJ/652/1715
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present RIz photometry of four consecutive transits of the newly discovered exoplanet XO-1b. We improve on the estimates of the transit parameters, finding the planetary radius to be R_P_=1.184^0.028^_0.018_R_J_, and the stellar radius to be R*=0.928^+0.018^_0.013_R_{sun}_, assuming a stellar mass of M*=(1.00+/-0.03)M_{sun}_.
2026. Four transits of WASP-4b
- ID:
- ivo://CDS.VizieR/J/ApJ/733/127
- Title:
- Four transits of WASP-4b
- Short Name:
- J/ApJ/733/127
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present photometry of four transits of the exoplanet WASP-4b, each with a precision of approximately 500ppm and a time sampling of 40-60s. We have used the data to refine the estimates of the system parameters and ephemerides. During two of the transits we observed a short-lived, low-amplitude anomaly that we interpret as the occultation of a starspot by the planet. We also found evidence for a pair of similar anomalies in previously published photometry. The recurrence of these anomalies suggests that the stellar rotation axis is nearly aligned with the orbital axis, or else the starspot would not have remained on the transit chord. By analyzing the timings of the anomalies we find the sky-projected stellar obliquity to be {lambda}=-1^+14^_-12_degrees. This result is consistent with (and more constraining than) a recent observation of the Rossiter-McLaughlin effect. It suggests that the planet migration mechanism preserved the initially low obliquity, or else that tidal evolution has realigned the system. Future applications of this method using data from the CoRoT and Kepler missions will allow spin-orbit alignment to be probed for many other exoplanets.
- ID:
- ivo://CDS.VizieR/J/A+A/633/A147
- Title:
- FQS. Galactic Plane CO survey
- Short Name:
- J/A+A/633/A147
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the Forgotten Quadrant Survey (FQS), an ESO large project that used the 12m antenna of the Arizona Radio Observatory to map the Galactic Plane in the range 220{deg}<l<240{deg}, and -2.5{deg}<b<0{deg}, both in ^12^CO(1-0), and ^13^CO(1-0), at a spectral resolution of 0.65km/s and 0.26km/s. We used the (1-0) transition of carbon monoxide to trace the molecular component of the interstellar medium. Our data set allows us to easily identify how the molecular dense gas is organised at different spatial scales: from the giant clouds with their denser filamentary networks, down to the clumps and cores that host the new-born stars and to obtain reliable estimates of their key physical parameters such as size and mass. We present the first release of the data of the FQS survey and discuss their quality. Spectra with 0.65km/s velocity channels have noise ranging from 0.8K to 1.3K for ^12^CO (1-0) and from 0.3K to 0.6K for ^13^CO (1-0). In this first paper, we used the ^12^CO (1-0) spectral cubes to produce a catalogue of 263 molecular clouds. The clouds are grouped in three main structures corresponding to the Local, Perseus, and Outer arms up to a distance of ~8.6kpc from the Sun. This is the first self-consistent statistical catalogue of molecular clouds of the outer Galaxy obtained with a subarcminute spatial resolution and therefore able to detect not only the classical giant molecular clouds, but also the small clouds and to resolve the cloud structure at the sub-parsec scale up to a distance of a few kiloparsec. We found two classes of objects: structures with sizes above a few parsecs that are typical molecular clouds and may be self-gravitating, and subparsec structures that cannot be in gravitational equilibrium and are likely transient or confined by external pressure. We used the ratio between the Herschel H2 column density and the integrated intensity of the CO lines to calculate the CO conversion factor and we found mean values of (3.3+/-1.4)x10^20^cm^-2^/(K.km/s) and (1.2+/-0.4)x10^21^cm^-2^/(K.km/s), for ^12^CO (1-0) and ^13^CO (1-0), respectively. FQS contributes to the general effort in producing a new generation of high-quality spectroscopic data for the Galactic Plane in the less studied third Galactic Quadrant, toward the outer Galaxy. FQS has produced a data-set of great legacy value, largely improving the data quality both in terms of sensitivity and spatial resolution over previous data sets.
- ID:
- ivo://CDS.VizieR/J/MNRAS/452/4307
- Title:
- From optical to infrared photometry of SN 2013dy
- Short Name:
- J/MNRAS/452/4307
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- SN 2013dy is a Type Ia supernova (SN Ia) for which we have compiled an extraordinary data set spanning from 0.1 to ~500d after explosion. We present 10 epochs of ultraviolet (UV) through near-infrared (NIR) spectra with Hubble Space Telescope/Space Telescope Imaging Spectrograph, 47 epochs of optical spectra (15 of them having high resolution), and more than 500 photometric observations in the BVrRiIZYJH bands. SN 2013dy has a broad and slowly declining light curve ({Delta}m_15_(B)=0.92mag), shallow SiII {lambda}6355 absorption, and a low velocity gradient. We detect strong CII in our earliest spectra, probing unburned progenitor material in the outermost layers of the SN ejecta, but this feature fades within a few days. The UV continuum of SN 2013dy, which is strongly affected by the metal abundance of the progenitor star, suggests that SN 2013dy had a relatively high-metallicity progenitor. Examining one of the largest single set of high-resolution spectra for an SN Ia, we find no evidence of variable absorption from circumstellar material. Combining our UV spectra, NIR photometry, and high-cadence optical photometry, we construct a bolometric light curve, showing that SN 2013dy had a maximum luminosity of 10.0^+4.8^_-3.8_x10^42^erg/s. We compare the synthetic light curves and spectra of several models to SN 2013dy, finding that SN 2013dy is in good agreement with a solar-metallicity W7 model.
- ID:
- ivo://CDS.VizieR/J/A+A/627/A140
- Title:
- FSRQ PKS 0346-27 light curves
- Short Name:
- J/A+A/627/A140
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this paper, we characterize the first-ray flaring episode of the flat-spectrum radio quasar PKS 034-27 (z=0.991), as revealed by Fermi-LAT monitoring data, and the concurrent multi-wavelength variability observed from radio through X-rays. We studied the long- and short-term flux and spectral variability from PKS 0346-27 by producing-ray light curves with different time binning. We complement theFermi-LAT data with multi-wavelength observations from the Atacama Large MillimeterArray (radio mm-band), the Rapid Eye Mount telescope (near-infrared) and Swift (optical-UV and X-rays). This quasi-simultaneous multi-wavelength coverage allowed us to construct time-resolved spectral energy distributions (SEDs) of PKS 0346-27 and compare the broadband spectral properties of the source between different activity states using a one-zone leptonic emission model. PKS 0346-27 entered an elevated-ray activity state starting from the beginning of 2018. The high-state continued through-out the year, displaying the highest fluxes in May 2018. We find evidence of short-time scale variability down to approximately 1.5 hours, which constrains the-ray emission region to be compact. The extended flaring period was characterized by a persistently harder spectrum with respect to the quiescent state, indicating changes in the broadband spectral properties of the source. This was confirmed by the multi-wavelength observations, which show a shift in the position of the two SED peaks by approximately two orders of magnitude in energy and peak flux value. As a result, the non-thermal jet emission completely outshines the thermal contribution from the dust torus and accretion disk during the high state. The broadband SED of PKS 0346-27 transitions from a typical low-Synchrotron-Peaked (LSP) to the Intermediate-Synchrotron-Peaked (ISP) class, a behavior previously observed in other flaring-ray sources. Our one-zone leptonic emission model of the high-state SEDs constrains the gamma-ray emission region to have a lower magnetic field, larger radius, and higher maximum electron Lorentz factors with respect to the quiescent SED. Finally, we note that the bright and hard-ray spectrum observed during the peak of flaring activity in May 2018 implies that PKS 0346-27 could be a promising target for future ground-based Cherenkov observatories such as the Cherenkov Telescope Array (CTA). The CTA could detect such a flare in the low-energy tail of its energy range during a high state such as the one observed in May 2018.
2030. FSVS Cluster Catalogue
- ID:
- ivo://CDS.VizieR/J/MNRAS/369/1334
- Title:
- FSVS Cluster Catalogue
- Short Name:
- J/MNRAS/369/1334
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05<z<0.9 with mean <z>=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z>0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.
