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1101. EROS-2 Long Period Variables in LMC
ID:
ivo://CDS.VizieR/J/A+A/536/A60
Title:
EROS-2 Long Period Variables in LMC
Short Name:
J/A+A/536/A60
Date:
21 Oct 2021
Publisher:
CDS
Description:
The EROS-2 survey has produced a database of millions of time series from stars monitored for more than six years, allowing us to classify some of their sources into different variable star types. Among the so-called, long period variables (LPVs), which are known to follow particular sequences in the period-luminosity diagram, we find long secondary period variables whose variability origin remains a matter of debate. We analyze data for the 856864 variable stars that have been discovered in the Large Magellanic Cloud (LMC) that are present in the EROS-2 database, to detect, classify, and characterize LPVs.
1102. 2016 eruption LC of the recurrent nova M31N 2008-12a
ID:
ivo://CDS.VizieR/J/ApJ/857/68
Title:
2016 eruption LC of the recurrent nova M31N 2008-12a
Short Name:
J/ApJ/857/68
Date:
21 Oct 2021
Publisher:
CDS
Description:
Since its discovery in 2008, the Andromeda galaxy nova M31N 2008-12a has been observed in eruption every single year. This unprecedented frequency indicates an extreme object, with a massive white dwarf and a high accretion rate, which is the most promising candidate for the single-degenerate progenitor of a Type Ia supernova known to date. The previous three eruptions of M31N 2008-12a have displayed remarkably homogeneous multiwavelength properties: (i) from a faint peak, the optical light curve declined rapidly by two magnitudes in less than two days, (ii) early spectra showed initial high velocities that slowed down significantly within days and displayed clear He/N lines throughout, and (iii) the supersoft X-ray source (SSS) phase of the nova began extremely early, six days after eruption, and only lasted for about two weeks. In contrast, the peculiar 2016 eruption was clearly different. Here we report (i) the considerable delay in the 2016 eruption date, (ii) the significantly shorter SSS phase, and (iii) the brighter optical peak magnitude (with a hitherto unobserved cusp shape). Early theoretical models suggest that these three different effects can be consistently understood as caused by a lower quiescence mass accretion rate. The corresponding higher ignition mass caused a brighter peak in the free-free emission model. The less massive accretion disk experienced greater disruption, consequently delaying the re-establishment of effective accretion. Without the early refueling, the SSS phase was shortened. Observing the next few eruptions will determine whether the properties of the 2016 outburst make it a genuine outlier in the evolution of M31N 2008-12a.
1103. ER Vulpeculae
ID:
ivo://CDS.VizieR/J/A+A/291/110
Title:
ER Vulpeculae
Short Name:
J/A+A/291/110
Date:
21 Oct 2021
Publisher:
CDS
Description:
(no description available)
1104. ESIS BVR catalog, ELAIS-S1
ID:
ivo://CDS.VizieR/J/A+A/451/881
Title:
ESIS BVR catalog, ELAIS-S1
Short Name:
J/A+A/451/881
Date:
21 Oct 2021
Publisher:
CDS
Description:
The ESO-Spitzer extragalactic Imaging Survey (ESIS) is the optical follow up of the Spitzer Wide-Area InfraRed Extragalactic (SWIRE) survey in the ELAIS-S1 area. The multiwavelength study of galaxy emission is the key to understand the interplay of the various components of galaxies and to trace their role in cosmic evolution. ESIS provides optical identification and colors of Spitzer IR galaxies and builds the bases for photometric redshift estimates. This paper presents B, V, R Wide Field Imager observations of the first 1.5 square degree of the ESIS survey. Data reduction includes astrometric calibration, illumination and color corrections. Synthetic sources are simulated in scientific and super-sky-flat images, with the purpose of estimating completeness and photometric accuracy for the survey. Number counts and color distributions are compared to literature observational and theoretical data, including non-evolutionary, PLE, evolutionary and semi-analytic Lambda-CDM galaxy models, as well as Milky Way stellar predictions. Object coordinates are defined with an accuracy as good as ~0.15" rms with respect to GSC 2.2; flux uncertainties are ~2, 10, 20% at mag. 20, 23, 24 respectively (Vega); we reach 95% completeness at B, V~25 and R~24.5. ESIS galaxy number counts are in good agreement with previous works and are best reproduced by evolutionary and hierarchical Lambda-CDM scenarios.
1105. ESO Distant Cluster Survey, EDisCS
ID:
ivo://CDS.VizieR/J/A+A/444/365
Title:
ESO Distant Cluster Survey, EDisCS
Short Name:
J/A+A/444/365
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the ESO Distant Cluster Survey (EDisCS) a survey of 20 distant galaxy clusters with redshifts ranging from 0.4 to 0.8. Candidate clusters were chosen from among the brightest objects identified in the Las Campanas Distant Cluster Survey (LCDCS), half with estimated redshift z_est_~0.5 and half with z_est_~0.8. They were confirmed by identifying red sequences in moderately deep two colour data from VLT/FORS2. For confirmed candidates we have assembled deep three-band optical photometry using VLT/FORS2, deep near-infrared photometry in one or two bands using NTT/SOFI, deep optical spectroscopy using VLT/FORS2, wide field imaging in two or three bands using the ESO Wide Field Imager, and HST/ACS mosaic images for 10 of the most distant clusters. This first paper presents our sample and the VLT photometry we have obtained. We present images, colour magnitude diagrams and richness estimates for our clusters, as well as giving redshifts and positions for the brightest cluster members. Subsequent papers will present our infrared photometry, spectroscopy, HST and wide-field imaging, as well as a wealth of further analysis and science results. Our reduced data become publicly available as these papers are accepted.
1106. ESO 1D reduced spectra
ID:
ivo://eso.org/ssap
Title:
ESO 1D reduced spectra
Short Name:
ESO SSAP
Date:
29 Mar 2022 09:14:37
Publisher:
European Southern Observatory
Description:
The ESO Simple Spectral Access service provides access to the 1D reduced spectra generated either by the principal investigators of ESO observations, or by an unattended ESO processing-pipeline that makes use of certified master calibrations. The spectra are FITS files adhering to the ESO Science Data Product standard, based on the Virtual Observatory Spectral Data Model standard (v1.0 for some spectra, and v2.0 for some others, use the VOCLASS FITS keyword to discern the two).
1107. ESO 362-G18 datacube
ID:
ivo://CDS.VizieR/J/A+A/614/A94
Title:
ESO 362-G18 datacube
Short Name:
J/A+A/614/A94
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present two-dimensional stellar and gaseous kinematics of the inner 0.7x1.2kpc^2^ of the Seyfert 1.5 galaxy ESO 362-G18, derived from optical (4092-7338{AA}) spectra obtained with the GMOS integral field spectrograph on the Gemini South telescope at a spatial resolution of 170 pc and spectral resolution of 36km/s. ESO 362-G18 is a strongly perturbed galaxy of morphological type Sa or S0/a, with a minor merger approaching along the NE direction. Previous studies have shown that the [OIII] emission shows a fan-shaped extension of ~10" to the SE. We detect the [OIII] doublet, [NII] and H{alpha} emission lines throughout our FOV. The stellar kinematics is dominated by circular motions in the galaxy plane, with a kinematic position angle of ~137{deg} and is centred approximately on the continuum peak. The gas kinematics is also dominated by rotation, with kinematic position angles ranging from 122{deg} to 139{deg}, projected velocity amplitudes of the order of 100km/s, and a mean velocity dispersion of 100km/s. A double-Gaussian fit to the [OIII]{lambda}5007 and H{alpha} lines, which have the highest signal to noise ratios of the emission lines, reveal two kinematic components: (1) a component at lower radial velocities which we interpret as gas rotating in the galactic disk; and (2) a component with line of sight (LOS) velocities 100-250km/s higher than the systemic velocity, interpreted as originating in the outflowing gas within the AGN ionization cone. We estimate a mass outflow rate of 7.4x10^-2^M_{sun}_/yr in the SE ionization cone (this rate doubles if we assume a biconical configuration), and a mass accretion rate on the supermassive black hole (SMBH) of 2.2x10^-2^M_{sun}_/yr. The total ionized gas mass within 84pc of the nucleus is 3.3x10^5^M_{sun}_; infall velocities of ~34km/s in this gas would be required to feed both the outflow and SMBH accretion.
1108. ESO Imaging Survey. CDF-S point sources
ID:
ivo://CDS.VizieR/J/A+A/384/81
Title:
ESO Imaging Survey. CDF-S point sources
Short Name:
J/A+A/384/81
Date:
21 Oct 2021
Publisher:
CDS
Description:
This paper describes the methodology currently being implemented in the EIS pipeline for analysing optical/infrared multi-colour data. The aim is to identify different classes of objects as well as possible undesirable features associated with the construction of colour catalogues. The tools developed are used for a preliminary analysis of the multi-colour point source catalogue constructed from the optical/infrared imaging data obtained for the Chandra Deep Field South (CDF-S). These data are publicly available, representing the first installment of the ongoing EIS Deep Public Survey.
1109. ESO Imaging Survey. IV.
ID:
ivo://CDS.VizieR/J/A+AS/137/75
Title:
ESO Imaging Survey. IV.
Short Name:
J/A+AS/137/75
Date:
21 Oct 2021
Publisher:
CDS
Description:
This paper presents preliminary lists of potentially interesting point-like sources extracted from multicolour data obtained for a 1.7 square degree region near the South Galactic Pole. The region has been covered by the ESO Imaging Survey (EIS) in B, V and I and offers a unique combination of area and depth. These lists, containing a total of 330 objects nearly all brighter than I~21.5, over 1. 27 square degrees (after removing some bad regions), are by-products of the process of verification and quality control of the object catalogs being produced. Among the colour selected targets are candidate very low mass stars/brown dwarfs (54), white-dwarfs (32), and quasars (244). In addition, a probable fast moving asteroid was identified. The objects presented here are natural candidates for follow-up spectroscopic observations and illustrate the usefulness of the EIS data for a broad range of science and for providing possible samples for the first year of the VLT.
1110. ESO TAP_CAT: a TAP service to query the astronomical catalogs generated by ESO observers, including the catalogs of the ESO Public Surveys.
ID:
ivo://eso.org/tap_cat
Title:
ESO TAP_CAT: a TAP service to query the astronomical catalogs generated by ESO observers, including the catalogs of the ESO Public Surveys.
Short Name:
ESO TAP_CAT
Date:
26 Jun 2024 14:26:53
Publisher:
European Southern Observatory
Description:
TAP_CAT is the ESO Science Archive service that provides programmatic access onto the astronomical catalogues produced by the principal investigators of ESO programmes. The Table Access Protocol (TAP) lets you execute queries against our astronomical catalogues. The queries must adhere to the Astronomical Data Query Language (ADQL, IVOA standard). Table Upload is not currently supported, though it is foreseen for a next release. This service provides limited support for spatial queries; only CONTAINS and CIRCLE are supported, as in this example: CONTAINS(point('', catalog_rightascension, catalog_declination), CIRCLE('', user_defined_rightascension, user_defined_declination, userdefined_radius))= 1. Please note that CONTAINS(...)=0 is not supported. A sister service (Catalog Facility: https://www.eso.org/qi) provides a web interface to the same collection of catalogues; the web interface implements a well-defined but limited query model, while instead TAP_CAT provides full ADQL support, allowing users to build their own query constraints using expressions, combining different columns, or using boolean operators (NOT, OR, etc.). A sibling service (TAP_OBS, endpoint: http://archive.eso.org/tap_obs) exists and can be used to query the raw and reduced data, and the atmospheric measurements taken at the La Silla Paranal Observatory (including APEX).