- ID:
- ivo://CDS.VizieR/J/A+A/384/925
- Title:
- Compiled catalog of stellar data of Miras
- Short Name:
- J/A+A/384/925
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Compiled Catalogue of Mira variables is a result of a merge of the 4th edition of the General Catalogue of Variable Stars (GCVS-4) <II/214A> and present-day high-precision catalogues of space (Hipparcos-Tycho family: Hipparcos <I/239>, Tycho-1 <I/239>, Tycho-2 <I/259>, ACT RC <I/246>, TRC <I/250>) and ground-based (CMC11 <I/256>, PPM-N <I/146>, PPM-S <I/193>, PPM-add <I/208>, Kharchenko 1992) data. The catalogue contains 1103 Miras. Equatorial coordinates were taken from the source catalogues in accordance with the priority: Hipparcos, Tycho-2, Tycho-1, CMC11, PPM, Kharchenko 1992. The proper motions of 1041 Miras are calculated as mean weighted values of source data reduced to the Hipparcos system. The radial velocities of 786 Miras were taken from nine catalogues and lists of Feast (1963MNRAS.125..367F, 1966MNRAS.132..495F), Smak and Preston (1965ApJ...142..943S), Perry and Bidelman (1965PASP...77..214P), Feast et al. (1972MNRAS.158...23F), Dean (1976AJ.....81..364D), Barnes and Fekel (1977Obs....97....1B), Feast et al. (1980MNRAS.190..227F), Barbier-Brossat and Figon (2000) <III/213>, and are given with respect of the absorption lines. For those radial velocities, which were determined from emission lines the correction has been made along with Ikaunieks (1971) relation: VR(abs) - VR(em) = 0.035 * Period. For 724 Miras both proper motions and radial velocities are available. The stars in the Compiled Catalogue are sorted in the same order as in the General Catalogue of Variable Stars.
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- ID:
- ivo://CDS.VizieR/J/BaltA/9/646
- Title:
- Compiled Catalogue of Mira-type stars
- Short Name:
- J/BaltA/9/646
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Compiled Catalogue of 1103 Mira type stars is created on the basis of the 4-th edition of the General Catalogue of Variable Stars (GCVS-4, Cat. <II/214>) and present day large high-precision catalogues based on space (Hipparcos-Tycho family catalogues: Hipparcos, Tycho-1 <I/239>, Tycho-2 (<I/259>), ACT RC (Urban et al., 1998AJ....115.2161U), TRC (Cat. <I/250>) and ground-based (CMC11 <I/256>, PPM-N <I/146>, PPM-S <I/193>, PPM-add <I/206>, Kharchenko, 1992, Kinematics and physics of celestial bodies 8, 61) data. Equatorial coordinates were taken from the source catalogues in accordance with the following priority: Hipparcos, Tycho-2, Tycho-1, CMC11, PPM, Kharchenko 1992. The proper motions in the Hipparcos system are calculated for 1041 Miras as mean weighted values of the reduced data from the source catalogues. The radial velocities obtained from absorption lines for 786 Miras were taken from nine catalogues and lists of Feast (1963MNRAS.125..367F, 1966MNRAS.132..495F), Smak and Preston (1965ApJ...142..943S), Perry and Bidelman (1965PASP...77..214P), Feast et al. (1972MNRAS.158...23F), Dean (1976AJ.....81..364D), Barnes and Fekel (1977Obs....97....1B), Feast et al. (1980MNRAS.190..227F), Barbier-Brossat and Figon (2000, Cat. <III/213>). Some radial velocities were determined from emission lines and corrected using the following formula (Ikaunieks, 1971, Long period variable stars, Zinante, Riga): V_R(abs) - V_R(em) = 0.035 * Period. For 724 Miras both proper motions and radial velocities are available. Miras in the Compiled Catalogue are sorted in the same order as in GCVS-4.
- ID:
- ivo://CDS.VizieR/J/A+A/562/A24
- Title:
- Cool carbon stars in the halo and Fornax dSph
- Short Name:
- J/A+A/562/A24
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The population of cool carbon (C) stars located far from the galactic plane is probably made of debris of small galaxies such as the Sagittarius dwarf spheroidal galaxy (Sgr), which are disrupted by the gravitational field of the Galaxy. We aim to know this population better through spectroscopy, 2MASS photometric colours, and variability data. When possible, we compared the halo results to C star populations in the Fornax dwarf spheroidal galaxy, Sgr, and the solar neighbourhood. We first present a few new discoveries of C stars in the halo and in Fornax. The number of spectra of halo C stars is now 125. Forty percent show H{alpha} in emission. The narrow location in the JHK diagram of the halo C stars is found to differ from that of similar C stars in the above galaxies. The light curves of the Catalina and LINEAR variability databases were exploited to derive the pulsation periods of 66 halo C stars. A few supplementary periods were obtained with the TAROT telescopes. We confirm that the period distribution of the halo strongly resembles that of Fornax, and we found that it is very different from the C stars in the solar neighbourhood. There is a larger proportion of short-period Mira/SRa variables in the halo than in Sgr, but the survey for C stars in this dwarf galaxy is not complete, and the study of their variability needs to be continued to investigate the link between Sgr and the cool halo C stars.
- ID:
- ivo://CDS.VizieR/III/282
- Title:
- CoRoT Bright Stars Catalogue with variability classes
- Short Name:
- III/282
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- The CoRoT bright stars catalogue describes the 143 different objects observed during the mission, in the "bright star" field of CoRoT, and their major properties. The almost continuous observations lasted between 20 and 156 days, with a regular 32s sampling time.
- ID:
- ivo://CDS.VizieR/B/corot
- Title:
- CoRoT observation log (N2-4.4)
- Short Name:
- B/corot
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- CoRoT, a space astronomy mission, has measured photometric micro-variability of stars from minutes to months (up to 150 days) with a high duty cycle (more than 90%). The mission was led by CNES in association with four French laboratories and 7 participating countries and agencies (Austria, Belgium, Brazil, Germany, Spain, and the ESA Science Programme). The satellite was composed of a PROTEUS platform (the 3rd in the series) and a unique instrument: a stellar rapid photometer. It was launched on December 27th 2006 by a Soyuz Rocket, from Baikonour. The mission has lasted almost 6 years (the nominal 3-year duration and a 3-year extension) and has observed more than 160 000 stars. It stopped sending data on November 2nd 2012. Two regions of the sky were accessible for long period of time: circles of 10 degrees centered on the equator around alpha=06:50 and alpha=18:50. They were called the CoRoT eyes: the "anticenter" and the "center eye" (as they are approximately in these directions). Each pointing covers 1.4x2.8 square degrees within one of those CoRoT eyes. The original scientific objectives were focussed on the study of stellar pulsations (asteroseismology) to probe the internal structure of stars, and the detection of small exoplanets through their "transit" in front of their host star, and the measurement of their size. This lead to introduce two modes of observations, working simultaneously: - The "bright star" mode dedicated to very precise seismology of a small sample of bright and closeby stars - The "faint star" mode, observing a very large number of stars at the same time, to detect transits, which are rare events, as they imply the alignment of the star, the planet and the observer. The large amount of data gathered in this mode turned out to be extremely fruitful for many topics of stellar physics. Beyond these two initial objectives, CoRoT data revealed stellar variability associated with various other phenomena: granulation, rotational modulation by spots associated with magnetic activity, oblateness induced by a nearby companion star, ... The data of this CoRoT CDS archive correspond to the legacy release V4.4 of CoRoT N2 data. A complete description can be found in the "CoRoTN2versions_30sept2014.pdf" document available on the vizier ftp as well as on project websites listed in the "See also" field below. Other archives provide an access to the CoRoT data at different levels, or to complementary catalogues - the CoRoT IAS archive at idoc-corot.ias.u-psud.fr/ and mirrors of this archive at exoplanetarchive.ipac.caltech.edu/applications/ETSS/CoRoT_exo_index.html and at exoplanetarchive.ipac.caltech.edu/applications/ETSS/CoRoT_astero_index.html - archive at https://sipad-corot.cnes.fr/ or at the CoRoT IAS archive, but they require a deep understanding of the instrument and the observation conditions to be scientifically helpful. - Raw data N0 are available upon request at the CoRoT CNES archive. - Complementary data on the CoRoT targets, obtained through ground based complementary observations, can be found in :
- ID:
- ivo://CDS.VizieR/J/A+A/629/A94
- Title:
- CO spectra of 49 semi-regular variables
- Short Name:
- J/A+A/629/A94
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We aim to study the main properties of a volume-limited unbiased sample of well characterized semi-regular variables (SRs) in order to clarify important issues that need to be further explained, such as the formation of axially symmetric planetary nebulae (PNe) from spherical circumstellar envelopes (CSEs) that takes place during the mass loss process along the AGB phase. We present new high S/N IRAM 30m observations of the ^12^CO J=2-1, ^12^CO J=1-0, and ^13^CO J=1-0 lines, in a volume-limited sample of SRs for which the Hipparcos distances are between 100-500 pc and declinations above -25{deg}. We analyzed the data by characterizing the main properties of the CSEs. The ^12^CO J=2-1 data have been used to study the profiles, while the ^12^CO J=1-0 data have been used to estimate mass-loss rates for the complete sample. Moreover, the ^12^CO J=2-1 line has been used to determine the possible structures responsible for such profiles. We have classified the sources into four groups according to the different profiles and final gas expansion velocities. Type 1 and 2 profiles are broad and narrow symmetric lines, respectively. Type 1 profiles, furthermore, are more related to standard spherically symmetric envelopes already studied. Type 3 profiles, on the contrary, are strange profiles with very pronounced asymmetries. Type 4 profiles, finally, are those which show two different components: a narrow line profile superimposed on a broad pedestal component. We find that for sources which show this kind of profile, with two different components, the variation amplitude is very low, what means that these SRs do not have a well developed inner envelope differentiated from the outer one. Interestingly, we report a moderate correlation between mass-loss rates and ^12^CO J=1-0/^12^CO J=2-1 line intensity ratios for O-rich SRs, suggesting a different behaviour between C- and O-rich SRs. By using SHAPE+shapemol, we find a unified simple model based on an oblate spheroid, placed in different orientations, that may explain all the ^12^CO profiles in the sample, indicating that the gas expansion is, in general, predominantly equatorial. Moreover, in order to explain the type 4 profiles, we define an extra component which may somehow be a biconical structure or similar according to the structures already found in this kind of sources. Type 1 and 2 profiles, curiously, may also be explained by standard spherically symmetric envelopes, but often requiring anomalously low velocities. Type 3 and 4 profiles, however, need axial symmetry to be explained. We conclude that most circumstellar shells around SRs show axial, strongly non-spherical symmetry. More interferometric observations are needed in order to make firm conclusions about mass-loss processes and possible morphologies of SRs.
- ID:
- ivo://CDS.VizieR/J/MNRAS/459/1170
- Title:
- Coulour-Period relation for Cepheids
- Short Name:
- J/MNRAS/459/1170
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We compare mid-infrared (IR) 3.6 and 4.5{mu}m Warm Spitzer observations for Cepheids in the Milky Way and the Large and Small Magellanic Clouds. Using models, we explore in detail the effect of the CO rotation-vibration band-head at 4.6{mu}m on the mid-IR photometry. We confirm the temperature sensitivity of the CO band-head at 4.6{mu}m and find no evidence for an effect at 3.6{mu}m. We compare the ([3.6]-[4.5]) period-colour relations in the MW, LMC and SMC. The slopes of the period-colour relations for the three galaxies are in good agreement, but there is a trend in zero-point with metallicity, with the lowest metallicity Cepheids having redder mid-IR colours. Finally, we present a colour-[Fe/H] relation based on published spectroscopic metallicities. This empirical relation, calibrated to the metallicity system of Genovali et al., demonstrates that the ([3.6]-[4.5]) colour provides a reliable metallicity indicator for Cepheids, with a precision comparable to current spectroscopic determinations.
- ID:
- ivo://CDS.VizieR/J/MNRAS/469/3688
- Title:
- CSS Periodic Variable Star Catalogue
- Short Name:
- J/MNRAS/469/3688
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Here we present the results from our analysis of six years of optical photometry taken by the Siding Spring Survey (SSS). This completes a search for periodic variable stars within the 30,000 square degrees of the sky covered by the Catalina Surveys. The current analysis covers 81 million sources with declinations between -20 and -75 degrees with median magnitudes in the range 11<V<19.5. We find approximately 34,000 new periodic variable stars in addition to the ~9,000 RR Lyrae that we previously discovered in SSS data. This brings the total number of periodic variables identified in Catalina data to ~110,000. The new SSS periodic variable stars mainly consist of eclipsing binaries, RR Lyrae, LPVs, RS CVn stars, {delta} Scutis and Anomalous Cepheids. By cross-matching these variable stars with those from prior surveys, we find that ~90% of the sources are new discoveries and recover ~95% of the known periodic variables in the survey region. For the known sources, we find excellent agreement between our catalogue and prior values of luminosity, period and amplitude. However, we find many variable stars that had previously been misclassified. Examining the distribution of RR Lyrae, we find a population associated with the Large Magellanic Cloud (LMC) that extends more than 20 degrees from its center confirming recent evidence for the existence of a very extended stellar halo in the LMC. By combining SSS photometry with Dark Energy Survey data, we identify additional LMC halo RR Lyrae, thus confirming the significance of the population.
- ID:
- ivo://CDS.VizieR/J/ApJ/892/112
- Title:
- CTIO/DECam LCs for Galactic bulge variable stars
- Short Name:
- J/ApJ/892/112
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- With the advent of the Legacy Survey of Space and Time, time-domain astronomy will be faced with an unprecedented volume and rate of data. Real-time processing of variables and transients detected by such large-scale surveys is critical to identifying the more unusual events and allocating scarce follow-up resources efficiently. We develop an algorithm to identify these novel events within a given population of variable sources. We determine the distributions of magnitude changes (dm) over time intervals (dt) for a given passband f, p_f_^(dm|dt)^, and use these distributions to compute the likelihood of a test source being consistent with the population or being an outlier. We demonstrate our algorithm by applying it to the DECam multiband time-series data of more than 2000 variable stars identified by Saha+ (2019, J/ApJ/874/30) in the Galactic Bulge that are largely dominated by long-period variables and pulsating stars. Our algorithm discovers 18 outlier sources in the sample, including a microlensing event, a dwarf nova, and two chromospherically active RS CVn stars, as well as sources in the blue horizontal branch region of the color-magnitude diagram without any known counterparts. We compare the performance of our algorithm for novelty detection with the multivariate Kernel Density Estimator and Isolation Forest on the simulated PLAsTiCC data set. We find that our algorithm yields comparable results despite its simplicity. Our method provides an efficient way for flagging the most unusual events in a real-time alert-broker system.
- ID:
- ivo://CDS.VizieR/J/AJ/154/85
- Title:
- CTIO/DECam photometry of RR Lyrae stars in M5
- Short Name:
- J/AJ/154/85
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We characterize the absolute magnitudes and colors of RR Lyrae stars in the globular cluster M5 in the ugriz filter system of the Dark Energy Camera (DECam). We provide empirical period-luminosity (P-L) relationships in all five bands based on 47 RR Lyrae stars of the type ab and 14 stars of the type c. The P-L relationships were found to be better constrained for the fundamental-mode RR Lyrae stars in the riz passbands, with dispersions of 0.03, 0.02 and 0.02mag, respectively. The dispersion of the color at minimum light was found to be small, supporting the use of this parameter as a means to obtain accurate interstellar extinctions along the line of sight up to the distance of the RR Lyrae star. We found a trend of color at minimum light with a pulsational period that, if taken into account, brings the dispersion in color at minimum light to 0.016 mag for the (r-i), (i-z), and (r-z) colors. These calibrations will be very useful for using RR Lyrae stars from DECam observations as both standard candles for distance determinations and color standards for reddening measurements.
