Search

Start Over Capability Type Simple Cone Search
921. ARAUCARIA project : NGC 6822 Cepheid variables
ID:
ivo://CDS.VizieR/J/ApJ/647/1056
Title:
ARAUCARIA project : NGC 6822 Cepheid variables
Short Name:
J/ApJ/647/1056
Date:
21 Oct 2021
Publisher:
CDS
Description:
We have measured near-infrared magnitudes in the J and K bands for 56 Cepheid variables in the Local Group galaxy NGC 6822 with well-determined periods and optical light curves in the V and I bands. Using the template light-curve approach of Soszyski and coworkers (2005PASP..117..823S), accurate mean magnitudes were obtained from these data, which allowed us to determine with unprecedented accuracy the distance to NGC 6822 from a multi-wavelength period-luminosity solution in the VIJK bands.
922. ARAUCARIA project: NGC 300 Cepheid variables
ID:
ivo://CDS.VizieR/J/AJ/123/789
Title:
ARAUCARIA project: NGC 300 Cepheid variables
Short Name:
J/AJ/123/789
Date:
21 Oct 2021
Publisher:
CDS
Description:
We have conducted a survey for Cepheid variables in the Sculptor group spiral NGC 300. Based on observations obtained with the Wide-Field Camera at the 2.2m ESO/MPI telescope at the La Silla observatory in Chile during 29 nights spread over a 5.3 month interval. The telescope was equipped with the ESO mosaic Wide-Field Camera (WFI) consisting of eight 2048x4098 pixel arrays. The CCDs were separated by gaps of 23.8" and 14.3" in right ascension and declination, respectively. The total field of view was about 34'x33' with a scale of 0.238"/pixel. 117 Cepheids and 12 Cepheid candidates were found, which cover the period range from 115 to 5.4 days. We present a catalog that provides equatorial coordinates, period, time of maximum brightness, and intensity mean B and V magnitudes for each variable, and we show phased B and V light curves for all the Cepheids found. We also present the individual B and V observations for each Cepheid in our catalog. During our search we rediscovered all 18 previously known Cepheids and confirmed the Cepheid nature of three Cepheid candidates from the previous photographic survey of Graham (1984AJ.....89.1332G). Star V4 in Graham's list (1984AJ.....89.1332G), classified by him as an eclipsing binary, turns out to be another Cepheid. We find very good agreement between our photometry and that obtained by Freedman et al. (1992ApJ...396...80F) from ground-based CCD data for common stars. Using the earlier data together with our new data, we were able to significantly improve the periods for 15 Cepheids in our sample.
923. ARAUCARIA project : NGC 300 Cepheid Variables. II
ID:
ivo://CDS.VizieR/J/AJ/128/1167
Title:
ARAUCARIA project : NGC 300 Cepheid Variables. II
Short Name:
J/AJ/128/1167
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present VI data, derive improved periods and mean magnitudes for the variables, and construct period-luminosity relations in the V, I, and the reddening-independent V-I Wesenheit bands using 58 Cepheid variables with periods between 11 and 90 days.
924. Arcetri Catalog of H2O maser sources. Update.
ID:
ivo://CDS.VizieR/J/A+A/368/845
Title:
Arcetri Catalog of H2O maser sources. Update.
Short Name:
J/A+A/368/845
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a second update of the Arcetri Catalog of water masers (Comoretto et al., 1990A&AS...84..179C; Brand et al., 1994, Cat. <J/A+AS/103/541>). The present study reports the results of the observations carried out with the Medicina 32-m radiotelescope from January 1993 to April 2000 on a sample of 300 sources. This compilation consists of newly discovered maser sources that did not appear in the previous Arcetri Catalogs and is made of: a) detections from the literature, and b) unpublished detections obtained with the Medicina antenna. Overall, 83 out of 300 sources were detected. The detection rate is low (28%) and we attribute this result to the inclusion in our survey of a rather large number of spurious maser detections that have appeared in one particular paper. The observational parameters are reported in tabular form for all the 300 sources and the spectra of the detected masers are presented. We discuss the global properties of the complete Arcetri Catalog based on Comoretto et al. (1990A&AS...84..179C), Brand et al. (1994, Cat. <J/A+AS/103/541>) and the present observations, which now contains 1013 galactic water maser sources. Of these, 937 have an IRAS counterpart within 1 arcmin from the nominal position of the maser. We establish a classification scheme based on the IRAS flux densities which allows to distinguish between water masers associated with star forming regions and late-type stars. The Arcetri Catalog represents a useful data base for systematic studies of galactic water maser sources.
925. Arcetri Catalogue of H2O Maser Sources
ID:
ivo://CDS.VizieR/J/A+AS/103/541
Title:
Arcetri Catalogue of H2O Maser Sources
Short Name:
J/A+AS/103/541
Date:
21 Oct 2021
Publisher:
CDS
Description:
An update is presented of the Arcetri Atlas of water masers (Comoretto et al. 1990A&AS...84..179C). It contains the results of observations of water masers with the Medicina 32-m antenna. The observed sources were all discovered in the period 1989-1993, and were found either directly in the course of our own programs or were taken from the literature in which case they were re-observed at Medicina. We give the observed parameters of 214 sources in tabular form, and present all the spectra of the 141 detections.
926. Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog
ID:
ivo://nasa.heasarc/arcquincxo
Title:
Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog
Short Name:
ARCQUINCXO
Date:
21 Feb 2025
Publisher:
NASA/GSFC HEASARC
Description:
The Galactic centre (GC) provides a unique laboratory for a detailed examination of the interplay between massive star formation and the nuclear environment of our Galaxy. Here are presented some of the results from a 100-ks Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of the Arches and Quintuplet star clusters in the form of a catalog of 244 point-like X-ray sources detected in the observation. The deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster. This table was created by the HEASARC in July 2007 based on &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/371/38"&gt;CDS Catalog J/MNRAS/371/38&lt;/a&gt; file table1.dat. This is a service provided by NASA HEASARC .
927. Arches cluster: IR phot., extinction and masses
ID:
ivo://CDS.VizieR/J/A+A/556/A26
Title:
Arches cluster: IR phot., extinction and masses
Short Name:
J/A+A/556/A26
Date:
21 Oct 2021
Publisher:
CDS
Description:
The Galactic Center is the most active site of star formation in the Milky Way Galaxy, where particularly high-mass stars have formed very recently and are still forming today. However, since we are looking at the Galactic Center through the Galactic disk, knowledge of extinction is crucial to study this region. The Arches cluster is a young, massive starburst cluster near the Galactic Center. We observed the Arches cluster out to its tidal radius using Ks-band imaging obtained with NAOS/CONICA at the VLT combined with Subaro/Cisco J-band data to gain a full understanding of the cluster mass distribution. We show that the determination of the mass of the most massive star in the Arches cluster, which had been used in previous studies to establish an upper-mass limit for the star formation process in the Milky Way, strongly depends on the assumed slope of the extinction law. Assuming the two regimes of widely used infrared extinction laws, we show that the difference can reach up to 30% for individually derived stellar masses and {Delta}AKs~1 magnitude in acquired Ks-band extinction, while the present mass function slope changes by ~0.17dex. The present-day mass function slope derived assuming the Nishiyama et al. (2009) extinction law increases from a flat slope of {alpha}-Nishi=-1.50+/-0.35 in the core (r<0.2pc) to {alpha}-Nishi=-2.21+/-0.27 in the intermediate annulus (0.2<r<0.4pc), where the Salpeter slope is -2.3. The present-day mass function steepens to {alpha}-Nishi=-3.21+/-0.30 in the outer annulus (0.4<r<1.5pc), indicating that the outer cluster region is depleted of high mass stars. This picture is consistent with mass segregation due to the dynamical evolution of the cluster.
928. Arches cluster JVLA 6 and 10GHz images
ID:
ivo://CDS.VizieR/J/A+A/647/A110
Title:
Arches cluster JVLA 6 and 10GHz images
Short Name:
J/A+A/647/A110
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present high angular resolution radio observations of the Arches cluster in the Galactic centre, one of the most massive young clusters in the Milky Way. The data were acquired in two epochs and at 6 and 10 GHz with the Karl G. Jansky Very Large Array (JVLA). The rms noise reached is 3-4 times better than previous observations and we have almost doubled the number of known radio stars in the cluster. Nine of them have spectral indices consistent with thermal emission from ionised stellar winds. One is a confirmed wind colliding binary and two sources are ambiguous cases. Regarding variability, the radio emission appears to be stable on time scales of a few to ten years. Finally, we have showed that the number of radio stars can be used as a tool for constraining the age or mass of a cluster and also its mass function.
929. Arches Cross-matched Catalogue
ID:
ivo://arches/xmatch/cs
Title:
Arches Cross-matched Catalogue
Short Name:
Arches-Xmatch
Date:
03 Feb 2025 08:32:20
Publisher:
ARCHES - Astronomical Resource Cross-matching for High Energy Studies
Description:
Each of the archival catalogues used for the crossmatch is referenced by single letter: 3XMM: x, Galex: g, UCAC:u CMC: c, SDSS: s, UKIDSS LAS: l, KIDS GPS: k ALLWISE; w AKARI: a and FIRST_NVSS_COMBO: r
930. Architecture of A1386 and the Sloan Great Wall
ID:
ivo://CDS.VizieR/J/MNRAS/410/1837
Title:
Architecture of A1386 and the Sloan Great Wall
Short Name:
J/MNRAS/410/1837
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present new radial velocities from AAOmega on the Anglo-Australian Telescope for 307 galaxies (bJ < 19.5) in the region of the rich cluster Abell 1386. Consistent with other studies of galaxy clusters that constitute subunits of superstructures, we find that the velocity distribution of A1386 is very broad (21000-42000 km/s, or z = 0.08-0.14) and complex. The mean redshift of the cluster that Abell designated as number 1386 is found to be ~0.104. However, we find that it consists of various superpositions of line-of-sight components. We investigate the reality of each component by testing for substructure and searching for giant elliptical galaxies in each and show that A1386 is made up of at least four significant clusters or groups along the line of sight whose global parameters we detail. Peculiar velocities of brightest galaxies for each of the groups are computed and found to be different from previous works, largely due to the complexity of the sky area and the depth of analysis performed in the present work. We also analyse A1386 in the context of its parent superclusters: Leo A and especially the Sloan Great Wall. Although the new clusters may be moving towards mass concentrations in the Sloan Great Wall or beyond, many are most likely not yet physically bound to it.

Limit your search

more »

more »

more »

more »

more »

more »