AAVSO Photometric All-Sky Survey (APASS), underway since 2010,
covers the entire sky from 7.5 < V < 16.5 magnitude, and in the BVugrizY
bandpasses. A northern and a southern site are used, each with twin ASA
20cm astrographs and Apogee Aspen CG16m cameras, covering 2.9x2.9 square
degrees with 2.6arcsec pixels. Landolt and SDSS standards are used for
all-sky solutions, with typical 0.02mag calibration errors on the bright
end.
Data Release 10 is a complete reprocessing of all 500K images taken with
the system, including hundreds of nights not part of DR9. Sextractor is
used for star finding and centroiding; DAOPHOT is used for aperture
photometry; the astrometry.net plate-solving library is used for basic
astrometry, supplanted with more precise WCS that utilizes knowledge of the
optical train distortions. With these changes, DR10 includes many more
stars than prior releases.
More information is available at http://www.aavso.org/apass.
A Catalog of Galaxies in the Direction of the Perseus Cluster
Short Name:
pcc cone
Date:
23 Mar 2022 13:13:05
Publisher:
The GAVO DC team
Description:
This is a catalog of 5437 morphologically classified sources in the
direction of the Perseus galaxy cluster core, among them 496
early-type low-mass galaxy candidates. The catalog is primarily based
on V-band imaging data acquired with the William Herschel Telescope.
Additionally, we used archival Subaru multiband imaging data in order
to measure aperture colors and to perform a morphological
classification. The catalog reaches its 50 per cent completeness limit
at an absolute V-band luminosity of -12 mag and a V-band surface
brightness of 26 mag arcsec^-2 .
In addition to the published table, this service also contains cutout
images of the objects investigated.
A classifier for spurious astrometric solutions in Gaia EDR3
Short Name:
gedr3spur.main
Date:
23 Mar 2022 13:13:08
Publisher:
The GAVO DC team
Description:
This table contains estimates of the "fidelity" of Gaia eDR3
astrometric solutions, a measure of the likelihood the eDR3 solution
is physical rather than spurious obtained using a neural network
trained on a small, hand-selected sample.
A all-sky compilation of galactic stellar sources observed for OH
maser emission in the transitions at 1612, 1665, and 1667 MHz. The
database contains OH maser observations selected from the literature .
These observations belong to more than 6000 different objects. The
database consists of three tables: The main table ("masers"),
interferometric followup observations ("maps") and monitoring programs
("monitor").
A Database of Circumstellar OH Masers: Interferometric Followups
Short Name:
engels oh maps
Date:
23 Mar 2022 13:13:07
Publisher:
The GAVO DC team
Description:
A all-sky compilation of galactic stellar sources observed for OH
maser emission in the transitions at 1612, 1665, and 1667 MHz. The
database contains OH maser observations selected from the literature .
These observations belong to more than 6000 different objects. The
database consists of three tables: The main table ("masers"),
interferometric followup observations ("maps") and monitoring programs
("monitor").
A Database of Circumstellar OH Masers: Monitoring Programs
Short Name:
engels oh mon
Date:
23 Mar 2022 13:13:07
Publisher:
The GAVO DC team
Description:
A all-sky compilation of galactic stellar sources observed for OH
maser emission in the transitions at 1612, 1665, and 1667 MHz. The
database contains OH maser observations selected from the literature .
These observations belong to more than 6000 different objects. The
database consists of three tables: The main table ("masers"),
interferometric followup observations ("maps") and monitoring programs
("monitor").
This brief tutorial shows you how to quickly add proper motions and
photometry from Gaia to (almost) any object list using the Virtual
Observatory. The VO protocol most suited to this kind of this is TAP
("table access protocol") and lets you transfer data and queries to
database servers. In the example, we will be using TOPCAT as a client.
There is no lock-in to it: There are libraries and other tools
allowing an integration of TAP operations into arbitrary workflows –
that's what standards are about. Tutorial supplements apply the
techniques to Simbad, show how to use TAP from Python, and introduce
UCDs.
This course introduces advanced usage of Hierarchical Progressive
Surveys (HiPS) and Multi-Order Coverage (MOC) maps in Aladin. Using
this document, you will learn how to handle a problem like : “I have a
set of images. I would like to select regions in my observations that
are above a given threshold in another survey (e.g. at low
extinction), retrieve objects from very large catalogs (e.g. Gaia +
WISE) in these non-trivial shapes and not-necessarily-connected
regions, and combine them to visualise some quantities (e.g. color
color diagram).“
This catalogue is a simulation of the Gaia DR2 stellar content using
Galaxia (a tool to sample stars from a Besancon-like Milky Way model),
3d dust extinction maps and the latest PARSEC Isochrones. It is
mimicking the Gaia DR2 data model and an apparent magnitude limit of
g=20,7. Extinctions and photometry in different bands have also been
included in a supplementary table as well as uncertainty estimates
using a scaled nominal error model.
This tutorial shows how to use the CDS tools to gather information on
specific astronomical objects. The tutorial covers the search for
information on NGC 4039 in the CDS Portal, the search for data on NGC
4039 in Aladin, and the omparison of the coverages of Sky Surveys and
select interacting galaxies that have SDSS and GALEX data.
2007-2010 ANTARES search for cosmic neutrino point sources
Short Name:
antares10 cone
Date:
23 Mar 2022 13:13:09
Publisher:
The GAVO DC team
Description:
A time integrated search for point sources of cosmic neutrinos was
performed using the data collected from January 2007 to November 2010
by the ANTARES neutrino telescope. This dataset includes a total of
3058 events obtained during the effective livetime of 813 days.
This is legacy data. The most recently released data can be found at
ivo://org.gavo.dc/antares/q/cone.
2007-2012 ANTARES search for cosmic neutrino point sources
Short Name:
antares cone
Date:
23 Mar 2022 13:13:16
Publisher:
The GAVO DC team
Description:
A time integrated search for point sources of cosmic neutrinos was
performed using the data collected from January 2007 to November 2012
by the ANTARES neutrino telescope. This dataset includes a total of
5921 events obtained during the effective livetime of 1338 days.
This service is an extension of the Apparent Places of Fundamental
Stars (APFS) computing exact geocentric positions in both the CIO and
equinox systems to stars from the Gaia DR2 result catalogue.
This service is an extension of the Apparent Places of Fundamental
Stars (APFS) computing exact geocentric positions in both the CIO and
equinox systems to stars from the Gaia DR3 result catalogue.
This service is an extension of the Apparent Places of Fundamental
Stars (APFS) computing exact geocentric positions in both the CIO and
equinox systems to stars from the Hipparcos catalogue.
ARI katkat is a catalog of star catalogues
in the spirit of G. Teleki's catalog of star catalogs
(`1989BOBeo.140..131T`_ and references in there). It contains
2573 catalogs suitable for astrometric usage, starting with Flamsteed
(1835) and ending in the 1970ies. For almost all of them, there
is a column description file (as PDF, and unfortunately sometimes in
German) and the digitized content.
.. _1989BOBeo.140..131T: http://ads.g-vo.org/abs/1989BOBeo.140..131T
ARI's "Geschichte des Fixsternhimmels" is an attempt to collect all
astrometrically useful observations from before ca. 1970 in a way
comparable to what has been done to construct the FK* series of
fundamental catalogs. About 7e6 published positions are included.
In GAVO's DC, we provide tables of identified and non-identified stars
together with the master catalog that objects were identified against.
ARI's "Geschichte des Fixsternhimmels" is an attempt to collect all
astrometrically useful observations from before ca. 1970 in a way
comparable to what has been done to construct the FK* series of
fundamental catalogs. About 7e6 published positions are included.
In GAVO's DC, we provide tables of identified and non-identified stars
together with the master catalog that objects were identified against.
The catalogue ARIHIP has been constructed by selecting the 'best
data' for a given star from combinations of HIPPARCOS data with Boss'
GC and/or the Tycho-2 catalogue as well as the FK6. It provides 'best
data' for 90 842 stars with a typical mean error of 0.89 mas/year
(about a factor of 1.3 better than Hipparcos for this sample of
stars).
In this tutorial you will learn about asteroids, a very interesting
and current topic in our exploration of the Solar System and of
planetary formation. You will learn about their orbital
characteristics by querying a database.
Intermediate computer skills are recommended, as the tutorial requires
the (guided) query of online electronic databases and use of
histograms.
The VO client Aladin offers powerful facilities of creating an
astrometrical calibration to images lacking WCS (World Coordinate
System) information. This tutorial shows how to go about doing this
for an image of the Ring Nebula in Lyr.
Astrometric Microlensing Events Predicted from Gaia DR2
Short Name:
am lensing 2
Date:
23 Mar 2022 13:13:04
Publisher:
The GAVO DC team
Description:
From the Gaia DR2 catalogue we predict astrometric microlensing
events by foreground stars with high proper motion (µ_tot >150mas/yr)
passing a background source in the next decades. Using Gaia DR2
photometry we determine an approximate mass of the lens, which we use
to calculate the expected microlensing effects. This yields 3914
microlensing events by 2875 different lenses between 2010 and 2065
with expected shifts larger than 0.1 mas between the lensed and
unlensed positions of the source. 513 of those are expected to happen
between 2014.5 - 2026.5 and might be measured by Gaia. For 127 events
we also expect a magnification between 1 mmag and 3 mag.
Astrometric Microlensing Events Predicted from Gaia eDR3
Short Name:
am lensing 2
Date:
23 Mar 2022 13:13:11
Publisher:
The GAVO DC team
Description:
From the Gaia eDR3 catalogue we predict astrometric microlensing
events by foreground stars with high proper motion (μ > 100 mas/yr)
passing a background source in the next decades. Using Gaia DR3
photometry we determine an approximate mass of the lens, which we use
to calculate the expected microlensing effects. This yields 4842
microlensing events by 3791 different lenses between 2010 and 2066
with expected shifts larger than 0.1 mas between the lensed and
unlensed positions of the source. The past events might be interested
when analyzing the individual Gaia measurements). 685 of those are
expected to happen within the next decade (2021-2031). For 140 events
we also expect a magnification between 1 mmag and 0.6 mag.
A form to search the VAMDC species list published on the TAP service
at http://dc.g-vo.org/tap. Enter parts of species names or chemical
formulae here and get back matching names, inchis and inchikeys.
Extracted sources from the Bochum Galactic Disk Survey. We provide
mean photometry in U, B, V, z, r, and i bands. Note that sources in
different bands are not matched. Also, sources sitting in the regions
imaged in multiple fields have not been matched even within one band.
In i and r, BGDS light curves are available. See related services for
details.
1BIGB: First Brazil-ICRANet Gamma-Ray Blazar Catalogue
Short Name:
1BIGB SSAP
Date:
23 Mar 2022 13:13:03
Publisher:
The GAVO DC team
Description:
This catalog presents the 1-100 GeV spectral energy distribution (SED)
for a population of 148 high-synchrotron-peaked blazars (HSPs) recently
detected with Fermi-LAT as part of the
First Brazil-ICRANet Gamma-ray Blazar catalogue (1BIGB).
A series of two works describe details on the broadband analysis:
:bibcode:`2017A&A...598A.134A`, and the calculation of the
gamma-ray SEDs :bibcode:`2018MNRAS.480.2165A`.
The 1BIGB sample was originally selected from an excess signal in the
0.3-500 GeV band The flux estimates presented here are derived considering
PASS8 data, integrating over more than 9 years of Fermi-LAT observations. The
full broadband fit between 0.3-500 GeV presented in paper 1 for all sources
was reevaluated in paper 2, updating the power-law parameters with currently
The Bochum Galactic Disk Survey is an ongoing project to monitor the
stellar content of the Galactic disk in a 6 degree wide stripe
centered on the Galactic plane. The data has been recorded since
mid-2010 in Sloan r and i simultaneously with the RoBoTT Telecsope at
the Universitaetssternwarte Bochum near Cerro Armazones in the Chilean
Atacama desert. It contains measurements of about 2x10^7 stars over
more than seven years. Additionally, intermittent measurements in
Johnson UVB and Sloan z have been recorded as well.
This service exposes the light curves of stars produced by the Bochum
Galactic Disk Survey; several million light curves are provided in the
SDSS i and r bands. The lightcurves are published per-band and are
also available through obscore.
The Armagh-Dunsink-Harvard Becker-Schmidt Telescope was deployed at
Boyden Station, Maselspoort South Africa between 1965 and 1970. During
that time, astronomers from Bamberg, Heidelberg, Hamburg and Münster
took astronomical images there, with a focus on old star clusters, the
Magellanic clouds, and the southern milky way. This service provides
scans of the plates obtained.
Split spectra from the CALIFA DR3 cubes. This service serves one
spectrum each per pixel in each cube where there is at least one valid
spaxel. Where both V500 and COMB data is available, COMB spectra are
served. WARNING: The individual spectra are not independent. Also,
error estimates over wide spectral ranges based on the error estimates
served here are unreliable.
The Calar Alto Legacy Integral Field Area (CALIFA) survey provides
spatially resolved spectroscopic information for 667 galaxies, mainly
within the local universe (0.005 < z < 0.03).
CALIFA data was obtained using the PPAK integral field unit (IFU), with a
hexagonal field-of-view of 1.3 square arcmin, with a 100% covering factor
by adopting a three-pointing dithering scheme. has been taken in two
setups: V500 (6 Å bin size, 646 galaxies) and V1200 (2.3 Å bin size, 484
galaxies). A final product ("COMBO") combining both data sets, covering
3700-7500 Å at 6 Å bin size, is made availble for 484 galaxies.
CALIFA is a legacy survey, intended for the community. This is the (final)
Data Release 3.
The overall goal of this tutorial is to become familiar with VOSpec.
For that, we are going to build the Spectral Energy Distribution (SED)
of two Herbig Ae/Be stars, compare them and categorise them as group 1
or group 2 Herbig Ae/Be stars.
This tutorial uses SPLAT-VO to search the VO registry for spectra of
galaxies and quasars. From the obtained spectra, the Hydrogen Lyman
Alpha line will be used to compute redshift and velocity
Within this intermediate use case you learn about supernovae (see
also the tutorial “Distance to the Crab Nebula“,
ivo://edu.euro-vo.org/tutorials/08_m1_distance) and determine the
celestial coordinates of a just discovered candidate supernova on an
provided image without astrometric calibration. This use case provides
a glimpse of an activity that is representative of the practical tasks
that astronomers have to perform when they analyze data.
Coordinated microlensing survey observations with Kepler K2/C9 using
VST
Short Name:
k2c9vst ssap
Date:
23 Mar 2022 13:13:09
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.
Differences between UCAC3 and PPMXL in positions and proper
motions, on
an all-sky one-degree grid. At each gridpoint we give the
differences X(PPMXL)- X(UCAC3) averaged over all stars in
a sqrt(2)/2-degrees environment around the gridpoint given. The
corrections given here should bring UCAC3 based astrometry to the ICRS.
Differences between USNO-B and PPMXL in positions and proper
motions, on
an all-sky one-degree grid. At each gridpoint we give the
differences X(PPMXL)- X(USNO-B1.0) averaged over all stars in
a sqrt(2)/2-degrees environment around the gridpoint given. The
corrections given here should bring USNO-B based astrometry to the ICRS.
The publication software DaCHS comes with a preconfigured authority
x-unregistred. Before version 2.3, it would let records with this null
authority into the VO. This authority's exclusive purpose is to let us
delete any such records.
Data Discovery Using the Virtual Observatory Registry
Date:
14 Mar 2023 10:41:41
Publisher:
The GAVO DC team
Description:
There are many ways to access registry data. A fairly powerful one is
the Web Interface to the Relational Registry (WIRR for short) at
http://dc.g-vo.org/WIRR To actually speak to the VO services
discovered, clients speaking the service's protocols are still
required. In this tutorial, Topcat plays that role. Starting from a
simple use case, we work up to investigating the Tully-Fisher relation
in different bands using independently discovered resources.
This is a deep optical mosaic of the Fornax cluster’s core, covering
1.6 square degrees. The data were acquired with ESO/MPG 2.2m/WFI,
using a transparent filter that nearly equals the no-filter throughput
and thus provides a high signal-to-noise ratio. Based on an
approximate conversion to V-band magnitudes, the unbinned and binned
mosaics (0.24 and 0.71 arcsec/pixel) reach a median depth of 26.6 and
27.8 mag/sq.arcsec, respectively.