VO Fresh

UVES/VLT spectra of white dwarfs (Koester+, 2009)

2012-04-26T11:56:14Z

Description: The spectra are compared with theoretical model atmospheres using a chi^2^ fitting technique.
Author(s): Koester D., Voss B., Napiwotzki R., Christlieb N., Homeier D., Lisker T., Reimers D., Heber U.
IVOA id: ivo://CDS.VizieR/J/A+A/505/441

Kepler planetary candidates. I. (Borucki+, 2011)

2012-04-24T12:24:28Z

Description: In the spring of 2009, the Kepler Mission commenced high-precision photometry on nearly 156000 stars to determine the frequency and characteristics of small exoplanets, conduct a guest observer program, and obtain asteroseismic data on a wide variety of stars. On 2010 June 15, the Kepler Mission released most of the data from the first quarter of observations. At the time of this data release, 705 stars from this first data set have exoplanet candidates with sizes from as small as that of Earth to larger than that of Jupiter. Here we give the identity and characteristics of 305 released stars with planetary candidates. Data for the remaining 400 stars with planetary candidates will be released in 2011 February. More than half the candidates on the released list have radii less than half that of Jupiter. Five candidates are present in and near the habitable zone; two near super-Earth size, and three bracketing the size of Jupiter. The released stars also include five possible multi-planet systems. One of these has two Neptune-size (2.3 and 2.5 Earth radius) candidates with near-resonant periods.
Author(s): Borucki W.J., Koch D.G., Basri G., et al.
IVOA id: ivo://CDS.VizieR/J/ApJ/728/117

CoRoT-fields IRa01, LRa01, LRa02 stars SpType (Sebastian+, 2012)

2012-04-24T12:00:45Z

Description: Spectroscopic classification for 2950 O-, B-, and A-type stars in the CoRoT-fields IRa01, LRa01, and LRa02. Stars are named by their CoRoT-identifier and Coordinates are given. The visual magnitudes were obtained with the Wide Field Camera filter-system of the Isaac Newton Telescope at Roque de los Muchachos Observatory on La Palma and can be converted into Landolt standards, as shown in Deleuil et al. (2009AJ....138..649D).
Author(s): Sebastian D., Guenther E.W., Schaffenroth V., Gandolfi D., Geier S., Heber U., Deleuil M., Moutou C.
IVOA id: ivo://CDS.VizieR/J/A+A/541/A34

Properties of OH/IR stars with IRAS LRS spectra (Chen+, 2001)

2012-04-23T23:28:48Z

Description: This table contains the selected from the literature sample of 1065 OH maser sources with IRAS identification and LRS spectra. The most important physical quantities of these sources are assembled and the list of related references together with the abbreviations used is attached.
Author(s): Chen P.S., Szczerba R., Kwok S., Volk K.
IVOA id: ivo://CDS.VizieR/J/A+A/368/1006

Master Catalogue towards the Magellanic Clouds (MC2) (Delmotte+ 2002)

2012-04-23T11:51:46Z

Description: The Master Catalogue of stars towards the Magellanic Clouds (MC2) is a multi-wavelength reference catalogue. The current paper presents the first results of the MC2 project. We started with a massive cross-identification of the two recently released near-infrared surveys: the DENIS Catalogue towards the Magellanic Clouds (DCMC) with more than 1.3 million sources identified in at least two of the three DENIS filters (I J Ks) and the 2nd Incremental Release of the 2MASS point source catalogue (J H Ks) covering the same region of the sky. Both point source catalogues provide an unprecedented wealth of data on the stellar populations of the Magellanic Clouds (MCs). The cross-matching procedure has been extended to optical wavelength ranges, including the UCAC1 (USNO) and GSC2.2 catalogues. New cross-matching procedures for very large catalogues have been developed and important results on the astrometric and photometric accuracy of the cross-identified catalogues were derived. The cross-matching of large surveys is an essential tool to improve our understanding of their specific contents. This study has been partly supported by the ASTROVIRTEL project that aims at improving access to astronomical archives as virtual telescopes. This work has been supported by ASTROVIRTEL, a project funded by the European Commission under FP5 Contract No. HPRI-CT-1999-00081.
Author(s): Delmotte N., Loup C., Egret D., Cioni M.-R., Pierfederici F.
IVOA id: ivo://CDS.VizieR/IV/33

13 eclipsing binaries times of minima (Zasche, 2012)

2012-04-23T11:44:51Z

Description: Main aim of this paper is the first light curve and apsidal motion analysis of thirteen eccentric eclipsing binaries and determination of their basic physical properties. All of the systems were studied by the method of period analysis of times of minima and the light curve analysis. Many new times of minima were derived and collected from the data obtained by the automatic, robotic or satellite telescopes. This allows us to study the apsidal motion in these systems in detail for the first time. From the light curve analysis the first rough estimations of the physical properties of these systems were obtained.
Author(s): Zasche P.
IVOA id: ivo://CDS.VizieR/J/AcA/62/97

SN 1987A 3mm image (Lakicevic+, 2012)

2012-04-23T09:07:42Z

Description: We observed the source at 3-mm wavelength with a 750-m configuration of the Australia Telescope Compact Array (ATCA). We compared the image with a recent 3-cm image and with archival X-ray images.
Author(s): Lakicevic M., Zanardo G., van Loon J.T., Smith-Staveley L., Potter T., Ng C.-Y., Geansler B.M.
IVOA id: ivo://CDS.VizieR/J/A+A/541/L2

Main-belt asteroids polarimetric survey. II. (Gil-Hutton+, 2012)

2012-04-23T09:00:19Z

Description: Results for the objects observed during the polarimetric survey of main-belt asteroids. The observations were carried out during different observing runs between May 2004 and November 2009 at the 2.15m telescope of the CASLEO, San Juan, Argentina, using the Torino and CASPROF polarimeters.
Author(s): Gil-Hutton R., Canada-Assandri M.
IVOA id: ivo://CDS.VizieR/J/A+A/539/A115

SN 1987A images at 350 and 870um (Lakicevic+, 2012)

2012-04-23T08:29:52Z

Description: We observed SN 1987A during July-September 2011 with the Atacama Pathfinder EXperiment (APEX), at a wavelength of 350um with the Submillimetre APEX Bolometer CAmera (SABOCA) and at 870um with the Large APEX BOlometer CAmera (LABOCA). The 350-um image has superior angular resolution (8") over that of the Herschel Space Observatory 350-um image (25"). The 870-um observation (at 20" resolution) is a repetition of a similar observation made in 2007.
Author(s): Lakicevic M., van Loon J.T., Stanke T., De Breuck C., Patat F.
IVOA id: ivo://CDS.VizieR/J/A+A/541/L1

CY Aqr multiband photometry: 2011 season (Sterken+, 2012)

2012-04-22T17:32:25Z

Description: The differential magnitudes of V* CY Aqr are presented in rgb2011.dat and sat.2011.dat. The times of maximum light of V* CY Aqr are given in tmax2011.dat.
Author(s): Sterken C., Wiedemair C., Munaro T., Rigo J., Durnwalder J., Kirchler A., Damini Hofer J., Schraffl F., Olsen E. H., Tuvikene T.
IVOA id: ivo://CDS.VizieR/J/other/JAD/18.2

CRIRES-POP: high resolution IR spectra library (Lebzelter+, 2012)

2012-04-22T16:08:44Z

Description: Online available are the high resolution spectra presented in Figs. 3 to 15 of this paper. More data of the library are available via the webpage of the CRIRES-POP project http://www.univie.ac.at/crirespop. For each target three pieces of spectra around 1280nm, 1640nm, and 4050nm, respectively, are stored in individual files. The file names give the HD number and the wavelength range, except for Barnard's star (Fig. 13) where we use the name V2500Oph as the star has no HD number.
Author(s): Lebzelter T., Seifahrt A., Uttenthaler S., Ramsay S., Hartman H., Nieva M.F., Pryzibilla N., Smette A., Wahlgren G.M., Wolff B., Hussain G.A.J., Kaeufl H.U., Seemann U.
IVOA id: ivo://CDS.VizieR/J/A+A/539/A109

FR II radio galaxies in SDSS (Koziel-Wierzbowska+, 2011)

2012-04-22T15:04:59Z

Description: We limited our search to radio sources present in the Cambridge Catalogues of Radio Sources: * 3C (Edge et al. 1959MmRAS..68...37E, Bennett 1962MmRAS..68..163B, Cat. VIII/1); * 4C (Pilkington & Scott 1965MmRAS..69..183P; Gower, Scott & Wills 1967MmRAS..71...49G, Cat. VIII/4); * 5C (Pearson 1975, Cat. J/MNRAS/171/475; Pearson & Kus 1978, J/MNRAS/182/273; Benn et al. 1982, J/MNRAS/200/747; Benn & Kenderdine 1991MNRAS.251..253B, Cat. VIII/30; Benn 1995, Cat. J/MNRAS/272/699); * 6C (Baldwin et al. 1985MNRAS.217..717B, Cat. VIII/18; Hales, Baldwin & Warner 1988MNRAS.234..919H, Cat. VIII/21, 1993MNRAS.263...25H, Cat. VIII/25; Hales et al. 1990MNRAS.246..256H, Cat. VIII/22, 1991MNRAS.251...46H, Cat. VIII/23, 1993MNRAS.262.1057H, Cat. VIII/24); * 7C (Hales et al. 2007MNRAS.382.1639H, Cat. VIII/84); * 8C (Rees 1990MNRAS.244..233R, Hales et al. 1995MNRAS.274..447H, Cat. VIII/31) and * 9C (Waldram et al. 2003, Cat. J/MNRAS/342/915), and using the SDSS CrossID we cross-identified them with the sample of 926246 galaxies from the SDSS DR7 main galaxy sample.
Author(s): Koziel-Wierzbowska D., Stasinska G.
IVOA id: ivo://CDS.VizieR/J/MNRAS/415/1013

Proper motion study of M55 stars (Zloczewski+, 2011)

2012-04-19T15:36:41Z

Description: The images of M55 analysed in this paper were selected from the data collected by the Cluster AgeS Experiment (CASE) project during the period 1997-2008. Observations were made with the 2.5-m du Pont telescope at Las Campanas Observatory. All images were obtained with the same detector and the same set of filters.
Author(s): Zloczewski K., Kaluzny J., Thompson I.B.
IVOA id: ivo://CDS.VizieR/J/MNRAS/414/3711

JHKs photometry of Sculptor dSph galaxy (Menzies+, 2011)

2012-04-19T15:26:16Z

Description: Observations were made with the SIRIUS camera on the Japanese-South African Infrared Survey Facility (IRSF) at SAAO, Sutherland.
Author(s): Menzies J.W., Feast M.W., Whitelock P.A., Matsunaga N.
IVOA id: ivo://CDS.VizieR/J/MNRAS/414/3492

FUV excess in early-type galaxies (Carter+, 2011)

2012-04-19T15:14:21Z

Description: We present surface photometry of a sample of 52 galaxies from the GALaxy Evolution eXplorer (GALEX) and Two-Micron All-Sky Survey (2MASS) data archives. These include 32 normal elliptical galaxies, 10 ellipticals with weak LINER or other nuclear activity and 10 star-forming ellipticals or early-type spirals. We examine the spatial distribution of the far-ultraviolet excess in these galaxies, and its correlation with dynamical and stellar population properties of the galaxies.
Author(s): Carter D., Pass S., Kennedy J., Karick A.M., Smith R.J.
IVOA id: ivo://CDS.VizieR/J/MNRAS/414/3410

Hubble Legacy Archive ACS grism data (Kuemmel+, 2011)

2012-04-19T13:39:46Z

Description: A public release of slitless spectra, obtained with ACS/WFC and the G800L grism, is presented. Spectra were automatically extracted in a uniform way from 153 archival fields (or "associations") distributed across the two Galactic caps, covering all observations to 2008. The ACS G800L grism provides a wavelength range of 0.55-1.00um, with a dispersion of 40{AA}/pixel and a resolution of ~80{AA} for point-like sources. The ACS G800L images and matched direct images were reduced with an automatic pipeline that handles all steps from archive retrieval, alignment and astrometric calibration, direct image combination, catalogue generation, spectral extraction and collection of metadata. The large number of extracted spectra (73,581) demanded automatic methods for quality control and an automated classification algorithm was trained on the visual inspection of several thousand spectra. The final sample of quality controlled spectra includes 47919 datasets (65% of the total number of extracted spectra) for 32149 unique objects, with a median i_AB_-band magnitude of 23.7, reaching 26.5 AB for the faintest objects. Each released dataset contains science-ready 1D and 2D spectra, as well as multi-band image cutouts of corresponding sources and a useful preview page summarising the direct and slitless data, astrometric and photometric parameters. This release is part of the continuing effort to enhance the content of the Hubble Legacy Archive (HLA) with highly processed data products which significantly facilitate the scientific exploitation of the Hubble data. In order to characterize the slitless spectra, emission-line flux and equivalent width sensitivity of the ACS data were compared with public ground-based spectra in the GOODS-South field. An example list of emission line galaxies with two or more identified lines is also included, covering the redshift range 0.2-4.6. Almost all redshift determinations outside of the GOODS fields are new. The scope of science projects possible with the ACS slitless release data is large, from studies of Galactic stars to searches for high redshift galaxies.
Author(s): Kuemmel M., Rosati P., Fosbury R., Haase J., Hook R.N., Kuntschner H., Lombardi M., Micol A., Nilsson K.K., Stoehr F., Walsh J.R.
IVOA id: ivo://CDS.VizieR/J/A+A/530/A86

MUSYC optical imaging in ECDF-S (Cardamone+, 2010)

2012-04-19T09:49:08Z

Description: We carried out a medium-band imaging campaign on the Subaru Telescope using the wide field-of-view camera Suprime-Cam. Observations were collected in six runs over 2 years, in 2006 January, February, and December and 2007 January, March, and December.
Author(s): Cardamone C.N., Van Dokkum P.G., Urry C.M., Taniguchi Y., Gawiser E., Brammer G., Taylor E., Damen M., Treister E., Cobb B.E., Bond N., Schawinski K., Lira P., Murayama T., Saito T., Sumikawa K.
IVOA id: ivo://CDS.VizieR/J/ApJS/189/270

M dwarfs activity and radial velocity (Gomes da Silva+, 2012)

2012-04-19T08:31:06Z

Description: Due to their low mass and luminosity, M dwarfs are ideal targets if one hopes to find low-mass planets similar to Earth by using the radial velocity (RV) method. However, stellar magnetic cycles could add noise or even mimic the RV signal of a long-period companion. Following our previous work that studied the correlation between activity cycles and long-term RV variations for K dwarfs we now expand that research to the lower-end of the main sequence. Our objective is to detect any correlations between long-term activity variations and the observed RV of a sample of M dwarfs. We used a sample of 27 M-dwarfs with a median observational timespan of 5.9 years. The cross-correlation function (CCF) with its parameters RV, bisector inverse slope (BIS), full-width-at-half- maximum (FWHM) and contrast have been computed from the HARPS spectrum. The activity index have been derived using the Na I D doublet. These parameters were compared with the activity level of the stars to search for correlations. We detected RV variations up to ~5m/s that we can attribute to activity cycle effects. However, only 36% of the stars with long-term activity variability appear to have their RV affected by magnetic cycles, on the typical timescale of ~6 years. Therefore, we suggest a careful analysis of activity data when searching for extrasolar planets using long-timespan RV data.
Author(s): Gomes da Silva, J., Santos, N. C., Bonfils, X., Delfosse, X., Forveille, T., Udry, S., Dumusque, X., Lovis, C.
IVOA id: ivo://CDS.VizieR/J/A+A/541/A9

Type Ia supernova rates with HST ACS (Kuznetsova+, 2008)

2012-04-18T08:39:56Z

Description: For this analysis, we use the HST GOODS data set collected in 2002-2003. In addition to the GOODS data, we use an HST sample collected in the spring and summer of 2004, which we hereafter call the 2004 Advanced Camera for Surveys (ACS) sample.
Author(s): Kuznetsova N., Barbary K., Connolly B., et al.
IVOA id: ivo://CDS.VizieR/J/ApJ/673/981

DA-white dwarfs from SDSS and UKIDSS (Girven+, 2011)

2012-04-17T16:37:06Z

Description: These tables show the objects from the spectroscopic and photometric-only samples in "spec.dat" and "phot.dat" respectively. The table ire.dat shows all objects classified as having an infrared excess from its SDSS and UKIDSS spectral energy distribution. Finally posqso.dat lists the objects believed to be quasars from their SDSS and UKIDSS spectral energy distribution.
Author(s): Girven J., Gansicke B.T., Steeghs D., Koester D.
IVOA id: ivo://CDS.VizieR/J/MNRAS/417/1210

WISE Preliminary Data Release (Cutri+ 2011)

2012-04-17T15:24:12Z

Description: The Wide-field Infrared Survey Explorer (WISE; see Wright et al. 2010AJ....140.1868W) is a NASA Medium Class Explorer mission that conducted a digital imaging survey of the entire sky in the 3.4, 4.6, 12 and 22um mid-infrared bandpasses (hereafter W1, W2, W3 and W4). WISE will produce and release to the world astronomical and educational communities and general public a digital Image Atlas covering the sky in the four survey bands, and a reliable Source Catalog containing accurate photometry and astrometry for over 300 million objects. The WISE Catalog and Atlas will enable a broad variety of research efforts ranging from the search for the closest stars and brown dwarfs to the most luminous galaxies in the Universe. WISE science data products will serve as an important reference data set for planning observations and interpreting data obtained with future ground and space-borne observatories, such as JWST. WISE was launched on 2009-12-14 from Vandenberg SLC2W.
Author(s): Cutri R.M., et al.
IVOA id: ivo://CDS.VizieR/II/307

Photometry and spectroscopy of MS 1054-03 members (Tran+, 2007)

2012-04-17T12:35:59Z

Description: In 1998 May, a 5'x6' mosaic of the MS 1054-03 field was taken with WFPC2 on HST. Six slightly overlapping pointings were taken in both the F606W and F814W filters. For most of our analysis, we use the photometry and morphological information derived from imaging taken with HST ACS. A 2x2 overlapping mosaic (5.8'x5.8') was taken in F775W and F850LP in 2002 December, and the same pattern executed in F606W in 2004 January/February. A detailed description of the ACS image reduction is presented in Blakeslee et al. (2006, Cat. ).
Author(s): Tran K.-V.H., Franx M., Illingworth G.D., Van Dokkum P., Kelson D.D., Blakeslee J.P., Postman M.
IVOA id: ivo://CDS.VizieR/J/ApJ/661/750

Probing the core of red giants (Mosser+, 2012)

2012-04-17T12:31:07Z

Description: Asymptotic mixed-modes parameters of the red giant oscillation spectra shown in the paper. Dnu is the large separation. numax indicates the central frequency of the oscillation power excess. DPi1 is the gravity period spacing, e_DPi1 its uncertainty, assuming that {epsilon}_g_ is fixed to 1/2. If Dpi1 changes too much along the mixed-mode spectrum, DPi1b gives the second possible value. q is the coupling factor, e_q its uncertainty. Mass and Rad are the asteroseismic estimates of the stellar mass and radius from scaling relations, using Teff from the Kepler Input Catalog (Brown et al. 2011, Cat. V/133). The division between RGB and clump stars is derived from Fig. 3; the limit between the primary and secondary clump stars is set at 1.8 solar mass.
Author(s): Mosser B., Goupil M.J., Belkacem K., Michel E., Stello D., Marques J.P., Elsworth Y., Barban C., Beck P.G., Bedding T.R., De Ridder J., Garcia R.A., Hekker S., Kallinger T., Samadi R., Stumpe M.C., Barclay T., Burke C.J.
IVOA id: ivo://CDS.VizieR/J/A+A/540/A143

Flux estimations of faint X-ray sources (Getman+, 2010)

2012-04-17T09:29:13Z

Description: X-ray sources with very few counts can be identified with low-noise X-ray detectors such as the Advanced CCD Imaging Spectrometer on board the Chandra X-ray Observatory. These sources are often too faint for parametric spectral modeling using well-established methods such as fitting with XSPEC. We discuss the estimation of apparent and intrinsic broadband X-ray fluxes and soft X-ray absorption from gas along the line of sight to these sources, using nonparametric methods. Apparent flux is estimated from the ratio of the source count rate to the instrumental effective area averaged over the chosen band. Absorption, intrinsic flux, and errors on these quantities are estimated from comparison of source photometric quantities with those of high signal-to-noise spectra that were simulated using spectral models characteristic of the class of astrophysical sources under study. The concept of this method is similar to the long-standing use of color-magnitude diagrams in optical and infrared astronomy, with X-ray median energy replacing color index and X-ray source counts replacing magnitude. Our nonparametric method is tested against the apparent spectra of ~2000 faint sources in the Chandra observation of the rich young stellar cluster in the M 17 HII region. We show that the intrinsic X-ray properties can be determined with little bias and reasonable accuracy using these observable photometric quantities without employing often uncertain and time-consuming methods of nonlinear parametric spectral modeling. Our method is calibrated for thermal spectra characteristic of stars in young stellar clusters, but recalibration should be possible for some other classes of faint X-ray sources such as extragalactic active galactic nuclei.
Author(s): Getman K.V., Feigelson E.D., Broos P.S., Townsley L.K., Garmire G.P.
IVOA id: ivo://CDS.VizieR/J/ApJ/708/1760

FeII emission in a sample of AGN spectra (Kovacevic+, 2010)

2012-04-17T07:05:04Z

Description: We present a study of optical FeII emission in 302 active galactic nuclei (AGNs) selected from the Sloan Digital Sky Survey. We group the strongest FeII multiplets into three groups according to the lower term of the transition (b^4^F, a^6^S, and a^4^G terms). These approximately correspond to the blue, central, and red parts, respectively, of the "iron shelf" around H{beta}. We calculate an FeII template that takes into account transitions into these three terms and an additional group of lines, based on a reconstruction of the spectrum of I Zw 1. This FeII template gives a more precise fit of the FeII lines in broad-line AGNs than other templates. We extract FeII, H{alpha}, H{beta}, [OIII], and [NII] emission parameters and investigate correlations between them. We find that FeII lines probably originate in an intermediate line region. We note that the blue, red, and central parts of the iron shelf have different relative intensities in different objects. Their ratios depend on continuum luminosity, FWHM H{beta}, the velocity shift of FeII, and the H{alpha}/H{beta} flux ratio. We examine the dependence of the well-known anti-correlation between the equivalent widths of FeII and [OIII] on continuum luminosity. We find that there is a Baldwin effect for [OIII] but an inverse Baldwin effect for the FeII emission. The [OIII]/FeII ratio thus decreases with L_{lambda}5100_. Since the ratio is a major component of the Boroson & Green Eigenvector 1 (EV1), this implies a connection between the Baldwin effect and EV1 and could be connected with AGN evolution. We find that spectra are different for H{beta} FWHMs greater and less than ~3000km/s, and that there are different correlation coefficients between the parameters.
Author(s): Kovacevic J., Popovic L.C., Dimitrijevic M.S.
IVOA id: ivo://CDS.VizieR/J/ApJS/189/15