- ID:
- ivo://CDS.VizieR/VI/128
- Title:
- Log of CGPS exposures
- Short Name:
- VI/128
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/ApJ/663/1021
- Title:
- Log of {omega} Cen scientific images
- Short Name:
- J/ApJ/663/1021
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a photometric investigation on HB, RGB, and MSTO stars in omega Cen = NGC 5139. The center of the cluster was covered with a mosaic of F435W, F625W, and F658N band data collected with HST ACS. The outer reaches were covered with a mosaic of U-, B-, V-, and I-band data collected with the 2.2 m ESO/MPI telescope. The final catalog includes ~1.7 million stars. We identified more than 3200 likely HB stars, the largest sample ever collected in a globular cluster.
- ID:
- ivo://CDS.VizieR/B/subaru
- Title:
- Log of Subaru Prime Focus Camera Exposures
- Short Name:
- B/subaru
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This database contains a log of the Subaru Prime Focus Camera (Suprime-Cam) exposures since April 2001. The data are regularly updated, and the last date of the log is written in "File Summary". Note that from this version of Nov. 2005, the data number is largely increased because those data with worse position determination (up to 30 arcsec error) are included. Suprime-Cam is an 80-mega pixels (10240 x 8192) mosaic CCD camera, for the wide-field prime focus of the 8.2m Subaru telescope. Suprime-Cam covers a field of view 34'x27', a unique facility among the 8-10m class telescopes, with a resolution of 0".202 per pixel. The focal plane consists of ten high- resistivity 2kx2k CCDs developed by MIT Lincoln Laboratory, which are cooled by a large Stirling-cycle cooler. The CCD readout electronics was designed to be scalable, which allows the multiple read-out of tens of CCDs. It takes 50 seconds to readout entire arrays. A filter-exchange mechanism of the jukebox type is designed that can hold up to ten large filters (205x170x15mm^3^). The wide-field corrector is basically a three-lens Wynne- type, but has a new type of atmospheric dispersion corrector. The corrector provides a flat focal plane and an un-vignetted field of view of 30' in diameter. The achieved co-planarity of the focal array mosaic is smaller than 30um peak-to-peak, which realizes mostly the seeing limited image over the entire field. The median seeing in the I_c-band, measured over one year and a half, is 0".61. The PSF anisotropy in Suprime-Cam images, estimated by stellar ellipticities, is about 2% under this median seeing condition. At the time of commissioning, Suprime-Cam had the largest survey speed, which is defined as the field of view multiplied by the primary mirror area of the telescope, among those cameras built for sub-arcsecond imaging. For details, see: Miyazaki et al., Publ. Astron. Soc. Japan 54, 833-853, 2002 (2002PASJ...54..833M)
- ID:
- ivo://CDS.VizieR/J/PASJ/65/119
- Title:
- Low-resolution NIR spectra of zodiacal light
- Short Name:
- J/PASJ/65/119
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This catalog contains the 278 low-resolution (R~20) near-infrared (1.8-5.3micron) spectra of diffuse sky covering a wide range of galactic and ecliptic latitudes with the Infrared Camera (IRC) on board AKARI before the exhaustion of liquid-helium (from September 2006 to May 2007). Advanced reduction methods specialized for the slit spectroscopy of diffuse sky spectra are developed for constructing this spectral catalog. Filter wheel of the IRC instrument has dark position to measure the dark current, and uncertainty due to dark current subtraction is estimated to be <3nW/m2/sr at 2micron (Tsumura & Wada, 2011PASJ...63..755T). Point sources brighter than mK(Vega)=19 were detected on the slit and masked for deriving the diffuse spectrum. It was confirmed that the brightness due to unresolved galactic stars under this detection limit is negligible (<0.5% of the sky brightness at 2.2 micron) by a Milky Way star count model (TRILEGAL; Girardi et al., 2005A&A...436..895G). Cumulative brightness contributed by unresolved galaxies can be estimated by the deep galaxy counts, being <4nW/m2/sr at K band in the case of limiting magnitude of mK=19 (Keenan et al., 2010ApJ...723...40K).
- ID:
- ivo://CDS.VizieR/VI/99
- Title:
- Merged Log of IUE Observations
- Short Name:
- VI/99
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The log contains a summary of all IUE Newly Extracted Spectra (INES), which resulted from a post-processing effort at Vilspa. It was constructed by using verified data from the IUE Final Archive Master Catalogue. The observations cover the whole life of the satellite, from March 1978 to September 1996.
- ID:
- ivo://CDS.VizieR/VI/75
- Title:
- Merged Log of IUE Observations
- Short Name:
- VI/75
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The log contains data from January 26, 1978 through Dec. 92. It is sorted by right ascension.
- ID:
- ivo://CDS.VizieR/J/A+A/418/869
- Title:
- M31-RV evolution (1942-1993)
- Short Name:
- J/A+A/418/869
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The photometric evolution of M31-RV has been investigated on 1447 plates of the Andromeda galaxy obtained over half a century with the Asiago telescopes. M31-RV is a gigantic stellar explosion that occurred during 1988 in the Bulge of M31 and that was characterized by the appearance for a few months of an M supergiant reaching M_bol_=-10. The 1988 outburst has been positively detected on Asiago plates, and it has been the only such event recorded over the period covered by the plates (1942-1993). In particular, an alleged previous outburst in 1967 is excluded by the more numerous and deeper Asiago plates, with relevant implication for the interpretative models of this unique event.
- ID:
- ivo://CDS.VizieR/J/ApJ/712/405
- Title:
- Multiwavelength observations of 3C 454.3 III.
- Short Name:
- J/ApJ/712/405
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report on 18 months of multiwavelength observations of the blazar 3C 454.3 (Crazy Diamond) carried out in the period 2007 July-2009 January. During the 2008 May-2009 January period, the source average flux was highly variable, with a clear fading trend toward the end of the period, from an average {gamma}-ray flux F_E>100MeV_>~200x10^-8^photons/cm^2^/s in 2008 May-June, to F_E>100MeV_~80x10^-8^photons/cm^-2^/s in 2008 October-2009 January. In 2007 July-August and 2008 May-June, 3C 454.3 was monitored by Rossi X-ray Timing Explorer (RXTE). We also carried out simultaneous Swift observations during all AGILE campaigns. Swift/XRT detected 3C 454.3 with an observed flux in the 2-10keV energy band in the range (0.9-7.5)x10^-11^erg/cm^2^/s and a photon index in the range {Gamma}_XRT_=1.33-2.04. In the 15-150keV energy band, when detected, the source has an average flux of about 5mCrab. GASP-WEBT monitored 3C 454.3 during the whole 2007-2008 period in the radio, millimeter, near-IR, and optical bands. The observations show an extremely variable behavior at all frequencies, with flux peaks almost simultaneous with those at higher energies. An analysis of 15GHz and 43GHz VLBI core radio flux observations in the period 2007 July-2009 February shows an increasing trend of the core radio flux, anti-correlated with the higher frequency data, allowing us to derive the value of the source magnetic field.
- ID:
- ivo://CDS.VizieR/VI/117
- Title:
- Observation Log from ASCA
- Short Name:
- VI/117
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- ASCA (Advanced Satellite for Cosmology and Astrophysics) is the fourth Japanese X-ray astronomy satellite launched on February 20, 1993 (see Tanaka et al., 1994PASJ...46L..37T) The collaboration between Japanese and US scientists has been carried out in the developments of the X-ray telescopes, the X-ray CCD cameras, and software. ASCA observed more than 3000 targets before stopping scientific observations as a consequence of a huge solar flare occured in mid July, 2000. ISAS continued monitoring operation until the ASCA reentered the atmosphere on March 2, 2001. Scientific instrumentation of ASCA consists of four X-ray telescopes and corresponding focal plane detectors. Focal plane detectors are two X-ray CCD cameras (SIS: Solid-state Imaging Spectrometers) and two Gas Imaging Spectrometers (GIS). With these detectors, ASCA covers the energy range of 0.5-10 keV. This catalogue is a copy of the ASCA Observation log from the Data ARchive and Transmission System (DARTS), provided by the PLAIN center at ISAS/JAXA, Japan. All the ASCA data have been public. The data is archived in a target-oriented (strictly speaking, observation-oriented) structure, i.e., all the data produced from an observation is put into a directory --- although some exceptions exist for observations in very early epoch. Each dataset includes telemetry data, data products (event files, images, energy spectra, light curves, etc.), and calibration data. ISAS provides the telemetry and calibration data, and ASCA data processing center in ADF (Astrophysics Data Facility) at NASA/GSFC reproduces the data products.
- ID:
- ivo://CDS.VizieR/J/A+AS/105/67
- Title:
- Optical spectroscopy of 1Jy, S4 and S5 sources
- Short Name:
- J/A+AS/105/67
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- (no description available)
