The Chandra X-ray Observatory is the U.S. follow-on to the Einstein
Observatory and one of NASA"s Great Observatories.
Chandra was formerly known as AXAF, the Advanced X-ray
Astrophysics Facility, but renamed by NASA in December, 1998.
Originally three instruments and a high-resolution mirror carried in
one spacecraft, the project was reworked in 1992 and 1993. The Chandra
spacecraft carries a high resolution mirror, two imaging detectors,
and two sets of transmission gratings. Important Chandra features are:
an order of magnitude improvement in spatial resolution, good
sensitivity from 0.1 to 10 keV, and the capability for high spectral
resolution observations over most of this range.
The Chandra Source Catalog (CSC) includes information about X-ray
sources detected in observations obtained using the Chandra X-ray
Observatory. Release 2.0 of the catalog includes 317,167 point,
compact, and extended sources detected in ACIS and HRC-I imaging
observations released publicly prior to the end of 2014.
Observed source positions and multi-band count rates are reported, as
well as numerous derived spatial, photometric, spectral, and temporal
calibrated source properties that may be compared with data obtained
by other telescopes. Each record includes the best estimates of the
properties of a source based on data extracted from all observations
in which the source was detected.
The Chandra Source Catalog is extracted from the CXC"s Chandra Data
Archive (CDA). The CXC should be acknowledged as the source of Chandra data.
For detailed information on the Chandra Observatory and datasets see:
http://cxc.harvard.edu/ for general Chandra information;
http://cxc.harvard.edu/cda/ for the Chandra Data Archive;
http://cxc.harvard.edu/csc/ for Chandra Source Catalog information.
This archive collects and re-publishes third-party, mostly amateur,
images of the Gaia astrometry satellite to complemement the Ground Based
Optical Tracking (GBOT) effort.
Until Gaia passivation, there is a temporary upload facility
at https://dc.g-vo.org/citigbot/q/upload/form.
Pic du Midi de Bigorre in the French Pyrenees is the place where coronagraphic images were first realized, by Bernard Lyot in the 1930s. Since then, the solar instruments at Pic du Midi regularly provide images of the solar disc, solar prominences and solar corona.
Coordinated microlensing survey observations with Kepler K2/C9 using
VST
Short Name:
k2c9vst ssap
Date:
27 Dec 2024 08:31:04
Publisher:
The GAVO DC team
Description:
The Kepler satellite has observed the Galactic center in a campaign
lasting from April until the end of June 2016 (K2/C9). The main
objective of the 99 hours for the microlensing program 097.C-0261(A)
using the ESO VLT Survey Telescope (VST) was to monitor the superstamp
(i.e., the actually downloaded region of K2/C9) in service mode for
improving the event coverage and securing some color-information. Due
to weather conditions, the majority of images were taken in the red
band. These are part of the present release.
The exact pointing strategy was adjusted to cover the superstamp with
6 pointings and to contain as many microlensing events from earlier
seasons as possible. In addition, a two-point dither was requested to
reduce the impact of bad pixels and detector gaps. Consequently, some
events were getting more coverage and have been observed with
different CCDs. The large footprint of roughly 1 square degree and the
complementary weather conditions at Cerro Paranal have lead to the
coverage of 147 events (this resource's events table), but ~60 of
those were already at baseline.
