- 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.
Number of results to display per page
Search Results
- ID:
- ivo://ar.nova/fcaglp2/q/ssa
- Title:
- WR 35a: A new double-lined spectroscopic binary (Gamen+, 2014, A&A, 562, 13) at NOVA
- Short Name:
- NOVA WR35a
- Date:
- 30 Dec 2015 14:50:29
- Publisher:
- Nova
- Description:
- Reduced spectra used in the paper entitled "WR 35a: A new double-lined spectroscopic binary", by R. Gamen et al. to appear in the A&A journal (2014).
- ID:
- ivo://xaovo/liujun/liujun/q
- Title:
- XAO AGN Flux Monitoring Data
- Short Name:
- liujun_web
- Date:
- 25 Jun 2024 10:32:03
- Publisher:
- Xinjiang Astronomical Observatory,CAS
- Description:
- Active Galactic Nuclei (AGNs) are extragalactic objects characterized by extremely complex physical processes and strong temporal flux variability over almost the whole electromagnetic spectrum, which play a very important role in studying the formation and evolution of galaxies, cosmology and many other astrophysical problems. Flux variability is one of the most remarkable observational characteristics of AGNs and the variability time scales are from minutes to dozens of years. Multi-wavelength flux monitoring is the main means to study the nature of AGN flux variability. In order to systematically study the total flux variability of AGNs in radio band, we launched a long-term program, which is called the quasi- Simultaneous Multiwavelength Monitoring of AGNs with the Nanshan 26-m radio telescope of Xinjiang Astronomical Observatory (XAO), namely SMMAN program. The monitoring data were acquired monthly with the cross-scan mode at C-band (4.8 GHz) and K-band (23.6 GHz) for a sample of about 100 AGNs selected from Fermi-LAT suvery. Additionally, we also conducted weekly monitoring observations or Intra-Day Vairibility (IDV) observations for some of flaring Blazars to reveal their more complex variability time scales.
- ID:
- ivo://xaovo/__system__/services/registry
- Title:
- XAO Data Center Registry
- Short Name:
- XAO DC Reg
- Date:
- 10 Oct 2018 04:13:56
- Publisher:
- The staff at the XAO Data Center
- Description:
- The publishing registry for the XAO Data Center.
- ID:
- ivo://xaovo/cross/q/match
- Title:
- XAO DC Custom Uploading Crossmatcher
- Short Name:
- xao_crossmatch
- Date:
- 25 Jun 2024 10:32:03
- Publisher:
- Xinjiang Astronomical Observatory,CAS
- Description:
- A plain positional crossmatch service that allows file and URL uploads to be crossmatched to DC-internal tables. In general, you want to use TAP for this kind of thing when it is available, but in a pinch it might come in handy. Larger catalogues that can be matched against include GAIA,PPMXL,ATNF Pulsar Catalog, and more.
- ID:
- ivo://xaovo/pul/pulsar/q
- Title:
- XAO Pulsar Data Query
- Short Name:
- Pulsar_web
- Date:
- 02 Jan 2025 14:01:21
- Publisher:
- Xinjiang Astronomical Observatory,CAS
- Description:
- The pulsar timing data were obtained with the Nanshan 25M radio telescope. Our observations, which commenced in January 2000, have been made using a dual-channel room-temperature receiver with a bandwidth of 320 MHz centered at 1540 MHz before June 2002. The de-dispersion was provided by a 2X128X2.5 MHz analog filter-bank. A cryogenic receiver was mounted in July 2002, which increases the sensitivity to 0.5 mJy. In January 2010, a digital filter-bank (DFB) system came into operation. The higher time resolution allows us to monitor about 280 pulsars, including ten millisecond-pulsars (MSP). The format of the DFB data is "Psrfit". The "psrchive" program could reads and analyzes the data. Timing observations of 74 pulsars have been regularly carried out between 2002 July to 2009 December. These 74 pulsars have been monitored approximately once every 9d using a dual-channel cryogenic system that receives orthogonal linear polarizations at the central observing frequency of 1540 MHz. The folded profiles obtained are released in format PSRFITS for timing analysis, the file name extension is .FTp. Users can enter "~*.FTp*" in "Product key" filed to search and download it. Non-public data could be used with the permission of Dr. Shengnan Sun (sunshengnan@xao.ac.cn), please send an email for your request.
497. XAO SF Data Query
- ID:
- ivo://xaovo/wugang/wugang/q
- Title:
- XAO SF Data Query
- Short Name:
- wugang_web
- Date:
- 25 Jun 2024 10:32:03
- Publisher:
- Xinjiang Astronomical Observatory,CAS
- Description:
- The molecular spectrum lines data include mainly ammonia and water masers lines at 1.3cm band, as well as formaldehyde and recombination lines at 6cm band observed towards both our Galactic plane and nearby molecular clouds and star-forming regions.
- ID:
- ivo://esavo/xmm/tap
- Title:
- XMM-Newton data and catalogues
- Short Name:
- XMM
- Date:
- 06 Feb 2025 14:20:23
- Publisher:
- European Space Agency
- Description:
- This service provides access to XMM-Newton data and catalogues generated by the ESA XMM mission hosted at the ESAC Science Data Centre
- ID:
- ivo://wfau.roe.ac.uk/xmm_dsa
- Title:
- XMM-Newton Serendipitous Source Catalogue (2XMM)
- Short Name:
- 2XMM
- Date:
- 23 Jan 2024 09:36:54
- Publisher:
- WFAU, Institute for Astronomy, University of Edinburgh
- Description:
- XMM is the second comprehensive catalogue of serendipitous X-ray sources from the European Space Agency's (ESA) XMM-Newton observatory. The 2XMM catalogue is the largest X-ray source catalogue ever produced, containing almost twice as many discrete sources as either the ROSAT survey or pointed catalogues. 2XMM complements deeper Chandra and XMM-Newton small area surveys, probing a much larger sky area.
500. XMM SUSS
- ID:
- ivo://mssl.ucl.ac.uk/xmmsuss_dsa/XMMSUSS
- Title:
- XMM SUSS
- Date:
- 25 Apr 2012 11:27:46
- Publisher:
- XMM at MSSL
- Description:
- The XMM-OM Serendipitous Ultra-violet Source Survey (SUSS) is a catalog of UV sources detected serendipitously by the Optical Monitor (OM) on-board the European Space Agency's (ESA's) XMM-Newton observatory. It has been created at the University College London's (UCL's) Mullard Space Science Laboratory (MSSL) on behalf of ESA and is a partner resource to the 2XMM serendipitous X-ray source catalogue. The catalog contains source detections drawn from 2,417 XMM-OM observations in up to three broad band UV filters made between 2000 February 24 and 2007 March 29. All datasets included were publicly available by 2007 May 01 but note that, due to screening criteria, not all public observations are included in this catalog. Taking account of substantial overlaps between observations, the net sky area covered independently is 29 - 54 square degreees, depending on UV filter. The primary content of the catalog is filter-dependent source positions and magnitudes, and these are accompanied by profile diagnostics and variability statistics. The XMM-OM SUSS catalog contains 753,578 UV source detections above a signal-to-noise threshold limit of 3-sigma which relate to 624,049 unique objects. A significant fraction of sources (12% - UVW2, 11% - UVM2, 11.% - UVW1) are visited more than once during XMM operation, and a large fraction of sources (38% - UVW2, 23% - UVM2, 22% - UVW1) are observed more than once per filter during an individual visit. UVW2, UVM2 and UVW1 refer to the filter bandpasses defined in the Source Properties: Filter Set section of the MSSL documentation for this catalog: <a href="http://www.mssl.ucl.ac.uk/~mds/XMM-OM-SUSS/SourcePropertiesFilters.shtml">http://www.mssl.ucl.ac.uk/~mds/XMM-OM-SUSS/SourcePropertiesFilters.shtml</a>. Consequently, the scope for science based on temporal source variability on timescales of hours to years is broad. The positional accuracy of the catalog detections is typically 1.0 arcsec (1-sigma confidence radius) with a median positional error of 0.67 arcsec. The median AB magnitude of the catalog detections in the three UV bands is 19.56 (UVW2), 20.23 (UVM2) and 20.69 (UVW1). 20% of sources have AB magnitudes fainter than 20.28 (UVW2), 20.97 (UVM2) and 21.54 (UVW1). As part of quality evaluation for the catalog, each field has been tested for astrometric accuracy and visually screened for cosmetic problems, compromising aspect anomalies, stray light, large extended sources and telemetry dropouts. Observations affected by these issues (11.2%) have been removed from the catalog sample. Furthermore, 2% of all observations were selected at random where each source in this sample was tested for falsehood, spuriousness and accuracy of quality flagging. The results of this detailed screening are included in the full documentation. The processing used to generate the catalog is based on the SAS8.0 pipeline developed for the pipeline reduction of all XMM observations. This version includes a number of significant improvements over the previous data processing system (as used by the SSC in routine processing of XMM-Newton data on behalf of ESA). These improvements include a more robust detection scheme for sources close to the limit of sky background, refined quality flagging and a higher success rate (90%) for refined aspect corrections.
