- ID:
- ivo://irsa.ipac/WISE/Catalog/Prelim
- Title:
- WISE Preliminary Release Catalogs
- Short Name:
- WISE-Prelim
- Date:
- 16 Mar 2017 01:00:00
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The WISE Preliminary Release includes data from the first 105 days of WISE survey observations, 14 January 2010 to 29 April 2010, that were processed with initial calibrations and reduction algorithms. Primary release data products include an Atlas of 10,464 calibrated, coadded Image Sets, a Source Catalog containing positional and photometric information for over 257 million objects detected on the WISE images, and an Explanatory Supplement that provides a user's guide to the WISE mission and format, content, characteristics and cautionary notes for the Release products. Ancillary release products include an archive of over 754,000 Single-exposure Image sets and database of over 2.2 billion source extractions from those images, and moving object tracklets identified as part of the NEOWISE program (Mainzer et al. 2011).
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/ApJ/787/126
- Title:
- WISE reduced proper motions and spectral types
- Short Name:
- J/ApJ/787/126
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present an analysis of high proper motion objects that we have found in a recent study and in this work with multi-epoch astrometry from the Wide-field Infrared Survey Explorer (WISE). Using photometry and proper motions from the Two Micron All-Sky Survey and WISE, we have identified the members of this sample that are likely to be late-type, nearby, or metal-poor. We have performed optical and near-infrared spectroscopy on 41 objects, from which we measure spectral types that range from M4-T2.5. This sample includes 11 blue L dwarfs and 5 subdwarfs; the latter were also classified as such in the recent study by Kirkpatrick and coworkers. Based on their spectral types and photometry, several of our spectroscopic targets may have distances of <20 pc with the closest at ~12 pc. The tangential velocities implied by the spectrophotometric distances and proper motions indicate that four of the five subdwarfs are probably members of the Galactic halo while several other objects, including the early-T dwarf WISE J210529.08-623558.7, may belong to the thick disk.
- ID:
- ivo://CDS.VizieR/J/AJ/154/163
- Title:
- WISE-selected candidate SFRs beyond the Outer Arm
- Short Name:
- J/AJ/154/163
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The outer Galaxy beyond the Outer Arm provides a good opportunity to study star formation in an environment significantly different from that in the solar neighborhood. However, star-forming regions in the outer Galaxy have never been comprehensively studied or cataloged because of the difficulties in detecting them at such large distances. We studied 33 known young star-forming regions associated with 13 molecular clouds at R_G_>=13.5 kpc in the outer Galaxy with data from the Wide-field Infrared Survey Explorer (WISE) mid-infrared all-sky survey (Wright et al. 2010AJ....140.1868W; Jarrett et al. 2011ApJ...735..112J). From their color distribution, we developed a simple identification criterion of star-forming regions in the outer Galaxy with the WISE color. We applied the criterion to all the WISE sources in the molecular clouds in the outer Galaxy at R_G_>=13.5 kpc detected with the Five College Radio Astronomy Observatory (FCRAO) ^12^CO survey of the outer Galaxy (Heyer et al. 1998ApJS..115..241H), of which the survey region is 102.49{deg}=<l=<141.54{deg}, -3.03{deg}=<b=<5.41{deg}, and successfully identified 711 new candidate star-forming regions in 240 molecular clouds. The large number of samples enables us to perform the statistical study of star formation properties in the outer Galaxy for the first time. This study is crucial to investigate the fundamental star formation properties, including star formation rate, star formation efficiency, and initial mass function, in a primordial environment such as the early phase of the Galaxy formation.
24784. WISE view of RV Tauri stars
- ID:
- ivo://CDS.VizieR/J/MNRAS/453/133
- Title:
- WISE view of RV Tauri stars
- Short Name:
- J/MNRAS/453/133
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a detailed study based on infrared (IR) photometry of all Galactic RV Tauri stars from the General Catalogue of Variable Stars (GCVS). RV Tauri stars are the brightest among the Population II Cepheids. They are thought to evolve away from the asymptotic giant branch (AGB) towards the white dwarf domain. IRAS detected several RV Tauri stars because of their large IR excesses and it was found that they occupy a specific region in the [12]-[25], [25]-[60] IRAS two-colour diagram. We used the all sky survey of Wide-field Infrared Survey Explorer to extend these studies and compare the IR properties of all RV Tauri stars in the GCVS with a selected sample of post-AGB objects with the goal to place the RV Tauri pulsators in the context of post-AGB evolution. Moreover, we correlated the IR properties of both the RV Tauri stars and the comparison sample with other observables like binarity and the presence of a photospheric chemical anomaly called depletion. We find that Galactic RV Tauri stars display a range of IR properties and we differentiate between disc sources, objects with no IR excess and objects for which the spectral energy distribution (SED) is uncertain. We obtain a clear correlation between disc sources and binarity. RV Tauri stars with a variable mean magnitude are exclusively found among the disc sources. We also find evidence for disc evolution among the binaries. Furthermore our studies show that the presence of a disc seems to be a necessary but not sufficient condition for the depletion process to become efficient.
- ID:
- ivo://wfau.roe.ac.uk/wise-dsa
- Title:
- WISE (Wide-field Infrared Survey Explorer)
- Date:
- 04 Dec 2019 13:43:24
- Publisher:
- WFAU, Institute for Astronomy, University of Edinburgh
- Description:
- NASA's Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010) mapped the sky at 3.4, 4.6, 12, and 22 μm (W1, W2, W3, W4) in 2010 with an angular resolution of 6.1", 6.4", 6.5", & 12.0" in the four bands. WISE achieved 5Ï? point source sensitivities better than 0.08, 0.11, 1 and 6 mJy in unconfused regions on the ecliptic in the four bands. Sensitivity improves toward the ecliptic poles due to denser coverage and lower zodiacal background.
- ID:
- ivo://wfau.roe.ac.uk/wise-dsa/ceaApplication
- Title:
- WISE (Wide-field Infrared Survey Explorer)
- Date:
- 30 May 2013 15:06:48
- Publisher:
- WFAU, Institute for Astronomy, University of Edinburgh
- Description:
- NASA's Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010) mapped the sky at 3.4, 4.6, 12, and 22 μm (W1, W2, W3, W4) in 2010 with an angular resolution of 6.1", 6.4", 6.5", & 12.0" in the four bands. WISE achieved 5Ï point source sensitivities better than 0.08, 0.11, 1 and 6 mJy in unconfused regions on the ecliptic in the four bands. Sensitivity improves toward the ecliptic poles due to denser coverage and lower zodiacal background.
- ID:
- ivo://CDS.VizieR/J/ApJ/792/129
- Title:
- WISE W1/W2 Tully-Fisher relation calibrator data
- Short Name:
- J/ApJ/792/129
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In order to explore local large-scale structures and velocity fields, accurate galaxy distance measures are needed. We now extend the well-tested recipe for calibrating the correlation between galaxy rotation rates and luminosities-capable of providing such distance measures-to the all-sky, space-based imaging data from the Wide-field Infrared Survey Explorer (WISE) W1 (3.4 {mu}m) and W2 (4.6 {mu}m) filters. We find a correlation of line width to absolute magnitude (known as the Tully-Fisher relation, TFR) of M_W1_^b,i,k,a^=-20.35-9.56(logW_mx_^i^-2.5) (0.54 mag rms) and M_W2_^b,i,k,a^=-19.76-9.74(logW_mx_^i^-2.5) (0.56 mag rms) from 310 galaxies in 13 clusters. We update the I-band TFR using a sample 9% larger than in Tully & Courtois (2012ApJ...749...78T). We derive M_l_^b,i,k^=-21.34-8.95(logW_mx_^i^-2.5) (0.46 mag rms). The WISE TFRs show evidence of curvature. Quadratic fits give M_W1_^b,i,k,a^=-20.48-8.36(logW_mx_^i^-2.5)+3.60(loglogW_mx_^i^-2.5)^2^ (0.52 mag rms) and M_W2_^b,i,k,a^=-19.91-8.40(logW_mx_^i^-2.5)+ 4.32(loglogW_mx_^i^ -2.5)^2^ (0.55 mag rms). We apply an I-band -WISE color correction to lower the scatter and derive M_Cw1_=-20.22-9.12(logW_mx_^i^-2.5) and M_Cw2_=-19.63-9.11(logW_mx_^i^-2.5) (both 0.46 mag rms). Using our three independent TFRs (W1 curved, W2 curved, and I band), we calibrate the UNION2 Type Ia supernova sample distance scale and derive H_0_=74.4+/-1.4(stat)+/-2.4(sys) km/s/Mpc with 4% total error.
- ID:
- ivo://CDS.VizieR/J/AJ/150/100
- Title:
- WISE YSO candidates near {sigma} and {lambda} Ori
- Short Name:
- J/AJ/150/100
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have conducted a sensitive search down to the hydrogen burning limit for unextincted stars over ~200 square degrees around Lambda Orionis and 20 square degrees around Sigma Orionis using the methodology of Koenig & Leisawitz (2014ApJ...791..131K; K14). From WISE and 2MASS data we identify 544 and 418 candidate young stellar objects (YSOs) in the vicinity of {lambda} and {sigma} respectively. Based on our followup spectroscopy for some candidates and the existing literature for others, we found that ~80% of the K14-selected candidates are probable or likely members of the Orion star-forming region. The yield from the photometric selection criteria shows that WISE sources with K_S_-w3>1.5mag and K_S_ between 10 and 12mag are most likely to show spectroscopic signs of youth, while WISE sources with K_S_-w3>4mag and K_s_>12 were often active galactic nuclei when followed up spectroscopically. The population of candidate YSOs traces known areas of active star formation, with a few new "hot spots" of activity near Lynds 1588 and 1589 and a more dispersed population of YSOs in the northern half of the HII region bubble around {sigma} and {epsilon} Ori. A minimal spanning tree analysis of the two regions to identify stellar groupings finds that roughly two-thirds of the YSO candidates in each region belong to groups of 5 or more members. The population of stars selected by WISE outside the MST groupings also contains spectroscopically verified YSOs, with a local stellar density as low as 0.5 stars per square degree.
- ID:
- ivo://CDS.VizieR/J/AJ/136/312
- Title:
- 2001-2006 WIYN binary stars speckle observations
- Short Name:
- J/AJ/136/312
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A total of 1067 speckle observations of 345 binary stars are presented. Of these, 161 are double stars first resolved by Hipparcos, 17 are resolved for the first time in the observations presented here, and 21 are stars previously discovered by our program and reported in earlier papers in the series. In 947 cases, a magnitude difference is reported along with the relative astrometry.
- ID:
- ivo://CDS.VizieR/J/AJ/117/548
- Title:
- 1997 WIYN binary stars speckle observations
- Short Name:
- J/AJ/117/548
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Two hundred seventy-seven position angle and separation measures of 154 double stars are presented. Three of the systems were previously unknown to be double, and 16 other systems were discovered earlier this decade by the Hipparcos satellite. Measures are derived from speckle observations taken with the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5 m telescope located at Kitt Peak, Arizona. Speckle images were obtained using two different imaging detectors, namely, a multianode microchannel array (MAMA) detector and a fast-readout CCD. A measurement precision study was performed on a sample of binaries with extremely well known orbits by comparing the measures obtained here to the ephemeris predictions. For the CCD, the root mean square (rms) deviation of residuals was found to be 3.5 milliarcseconds (mas) in separation and 12 in position angle, while the residuals of the MAMA data varied depending on the magnification used and seeing conditions but can be comparable or superior to the CCD values. In addition, the two cameras were compared in terms of the detection limit in total magnitude and magnitude difference of the systems under study. The MAMA system has the ability to detect some systems with magnitude differences larger than 3.5, although reliable astrometry could not be obtained on these objects. Reliable astrometry was obtained on a system of magnitude difference of 5.3 with the CCD system.
