- ID:
- ivo://CDS.VizieR/J/ApJ/518/262
- Title:
- CCD VIc Photometry of M30 Stars
- Short Name:
- J/ApJ/518/262
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The file contains VIc data of the globular cluster M30. All frames were taken using a 2048x2048 pixel CCD with pixels covering 0.44 arcseconds on a side, for a total field of approximately 15 arcminutes on a side. Data were taken on 1994 July 78 at the Cerro Tololo Inter-American Observatory (CTIO) 4m telescope. The data were calibrated against Landolt (1983, Cat. <II/118>) standard stars.
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- ID:
- ivo://CDS.VizieR/J/A+A/388/149
- Title:
- CCD Vilnius photometry of M56
- Short Name:
- J/A+A/388/149
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- CCD observations of field stars in an area north-east of the globular cluster M 56 were obtained in six bands of the Vilnius photometric system. The data sets cover a field of 9'x9.5'. An outline of the data pathway from observations to reduction via IRAF is outlined in this text. Photometry of 366 stars brighter than 18th V magnitude has been obtained and the analysis of the observational errors is discussed.
- ID:
- ivo://CDS.VizieR/J/MNRAS/497/1791
- Title:
- CCD Washington photometry of Antlia cluster
- Short Name:
- J/MNRAS/497/1791
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present an extension of our previous research on the early-type galaxy population of the Antlia cluster (d~35Mpc), achieving a total coverage of ~2.6deg^2^ and performing surface photometry for ~300 galaxies, 130 of which are new uncatalogued ones. Such new galaxies mainly fall in the low surface brightness (LSB) regime, but there are also some lenticulars (S0) which support the existence of unique functions that connect bright and dwarf galaxies in the scaling relations. We analyse the projected spatial distribution of galaxies up to a distance of ~800kpc from NGC 3268, the adopted centre, as well as the radial velocity distribution and the correlation between galaxy colour and effective radius with the projected spatial distribution. We also obtain the luminosity function of the early-type galaxies and the distribution of stellar masses using the T1-band magnitudes and adopted mass-luminosity ratios. Additionally, we correlate the central galaxy distribution with an X-ray emission map from the literature. Based on the analysis of the radial velocities and galaxy colour distributions, we find that galaxies redder than the colour-magnitude relation (CMR) have a velocity distribution strongly concentrated towards the values of the dominant galaxies and are homogeneously distributed throughout the cluster. Those bluer than the CMR, in turn, have a much more extended radial velocity distribution and are concentrated towards the centre of the cluster. We also identify 12 candidates to ultra diffuse galaxies (UDG), that seem to be split into two families, and speculate about their origins in the context of the cluster structure.
- ID:
- ivo://CDS.VizieR/J/A+A/385/793
- Title:
- Cepheids in Magellanic Clouds. II.
- Short Name:
- J/A+A/385/793
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The analysis of CCD observations of ten new suspected second overtone mode Cepheids in the SMC does not confirm the nature of such stars; most of them appear to be first overtone mode Cepheids. A careful analysis of the OGLE best second overtone mode candidates and of the second overtone component of double mode Cepheids in SMC and LMC has been performed in order to clarify the possible effects of a resonance between pulsation modes. There are some indications that such a resonance is indeed operating in these pulsators. A brief discussion of the effects of blending on the light curve shape is also reported, and the usefulness of the Fourier parameters as mode discriminators is discussed. The observations were performed with the direct CCD camera at the Dutch 0.91m telescope of La Silla (ESO) during three runs in November 1997 (6 nights), July 1998 (12 nights) and October 1998 (15 nights). The CCD detector was the ESO chip No. 33, which is a TEK CCD with 512x512 pixels, pixel size of 27{mu}m and spatial resolution of 0.44", providing a small field of view of 3.77'x3.77'. 8 fields were selected in order to observe the ten second overtone candidates.
- ID:
- ivo://CDS.VizieR/II/253A
- Title:
- Chandra Deep Field South: multi-colour data
- Short Name:
- II/253A
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Table 3 contains the object catalogue of the COMBO-17 CDFS field. The observations were carried out with the Wide Field Imager (WFI) at the MPG/ESO 2.2-m telescope on La Silla, Chile, between October 1999 and January 2001 in four independent observing runs. The field measures 31.5'x30', is centered on RA=03:32:25, DE=-27:48:50 and contains the Chandra Deep Field South. The table contains 63501 objects found on the deep R-band image cdfs_r.fit by SExtractor with S/N>3. The 5-{sigma} magnitude limit for point sources is Rmag=26.0. Morphological information from the SExtractor measurement is included. Multiple observations in different observing runs of six different filters allow the identification of variable objects. The table contains positions, flags and flux measurements in UBVRI and 12 optical medium-band filters. In addition, we include multi-colour classification, photometric redshifts, luminosity distances and a number of absolute restframe magnitudes in different filters (Johnson, Sloan, Bessell). cdfs_u.fit, cdfs_b.fit, cdfs_v.fit, cdfs_r.fit and cdfs_i.fit are coadded sumframes in UBVRI of the CDFS field. These sumframes are stacked from flat-fielded and cosmic-corrected individual images by applying only full pixel shifts. Therefore, the coordinate frames differ slightly between the images. The coordinates in Table 3 refer to image cdfs_r.fit. The images in BVRI are obtained from observations carried out in observing run D (Oct 1999, see also Note (11) in the byte-by-byte description of table3.dat) while the U-band image is obtained from observing run G (Jan 2001). The exposure times are 14400s (U), 5000s (B), 8400s (V), 15000s (R) and 7550s (I). The intensity levels are given in units of photons hitting the detector (already corrected for the gain of the CCD). The data included here supersede the table2.dat of the COMBO-17 published in 2001 (J/A+A/377/442)
- ID:
- ivo://CDS.VizieR/J/A+A/377/442
- Title:
- Chandra Deep Field South: R-band photometry
- Short Name:
- J/A+A/377/442
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Table2 is based on an object list that was created by applying SExtractor software to an R-band image coadded from 36 frames with 15070s total exposure time taken in October 1999 using the Wide Field Imager at the MPG/ESO 2.2-m telescope on La Silla, Chile. The field measures 31.5'x30', is centered on 03:32:25-27:48:50 and contains the Chandra Deep Field South. The average PSF is on the order of 0.75". The catalog contains 63501 objects found by SExtractor with S/N>3. It has not been cleaned for spurious detection of false objects arising from scattered light or diffraction spikes of extremely bright stars. Using this object list aperture magnitudes 'Bmag', 'Vmag' and 'Rmag' were measured on B-, V- and R-band images taken in October 1999. These are listed with its errors. Additionally an aperture magnitude 'R2mag' with its error is included that is taken from R-band imaging from February 2000 with an exposure time of 8440s taken in 21 frames, yielding a total exposure time in the R-band of 23510s=6.5h. The 10-sigma magnitude limits for point sources are Bmag=24.9, Vmag=24.6, Rmag=25.1 and R2mag=24.8. The aperture magnitudes were calculated by counting the flux in an aperture with a Gaussian weighting function of 1.3" width. The flux is scaled to the total flux expected for stars.
- ID:
- ivo://CDS.VizieR/J/A+A/310/933
- Title:
- C isotopic ratio in N- and SC-type stars
- Short Name:
- J/A+A/310/933
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a result of quantitative analysis of ^12^C/^13^C ratios in 62 N-type and 15 SC-type carbon stars. By the use of CCD as a detector we can obtain spectra of resolution ~20,000 with enough signal-to-noise ratios for a large number of carbon stars, for which ^12^C/^13^C ratios have not yet been derived. Carbon isotopic ratios are determined from lines of the CN red system around 8000A, based on the iso-intensity method and line-blanketed model atmospheres. The average of ^12^C/^13^C ratios in 62 N-type carbon stars is found to be 27+/-11 (standard deviation). The majority of the N-type carbon stars studied (about 85%) are found to have ^12^C/^13^C ratios less than 40, and the number of stars which have ^12^C/^13^C ratios larger than 40 is found to be relatively small. This result shows a marked contrast to some of the previous results that have shown the opposite distribution, namely, ^12^C/^13^C ratios mostly larger than 40 in N-type carbon stars. The average of ^12^C/^13^C ratios in 15 SC-type carbon stars is found to be 22+/-14 (standard deviation). Most of the SC-type carbon stars studied are found to have ^12^C/^13^C ratios larger than 10, while only three of them turn out to be ^13^C-rich. This is in contrast with the earlier classification based on low resolution spectra which classified them as J-type, that is, ^13^C-rich. The earlier temperature scale which classified SC-type carbon stars as the latest (C8-9) based on their strong NaI D lines can not be necessarily justified. The strong NaI D lines of SC stars should be attributed to the peculiar atmospheric structure due to C/O ratios very near to unity. The resulting ^12^C/^13^C ratios are partly consistent with the scenario in which M giants evolve through SC-type to N-type carbon stars, as ^12^C produced during the helium shell flash is added to the envelope.
- ID:
- ivo://CDS.VizieR/J/PAZh/41/27
- Title:
- Classical Cepheids BVIc observations
- Short Name:
- J/PAZh/41/27
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In 2013-2014, we obtained 14959 CCD frames in the BVIc photometric system for 170 classical Cepheids from the General Catalogue of Variable Stars. We performed our observations with the 76-cm telescope of the South African Astronomical Observatory (SAAO, South Africa) using the SBIG ST-10XME CCD camera. The tables of observations, the plots of light curves, and the current light elements are presented.
- ID:
- ivo://CDS.VizieR/J/AJ/139/2669
- Title:
- CL Aur BVRI light curves
- Short Name:
- J/AJ/139/2669
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the first extensive photometric results of CL Aur from our BVRI CCD photometry made on 22 nights from 2003 November to 2005 February. Fifteen new timings of minimum light were obtained. During the past 104yr, the orbital period has varied due to a periodic oscillation superposed on a continuous period increase. The period and semi-amplitude of the oscillation are about 21.6yr and 0.0133-day, respectively.
- ID:
- ivo://CDS.VizieR/J/other/Obs/131.315
- Title:
- CL Eri, CM Eri, CN Eri BVIc light curves
- Short Name:
- J/other/Obs/131.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A total of total of 1071 B, V, Ic-band CCD frames are taken for three GCVS RR Lyr-type variables (CL Eri, CM Eri, and CN Eri), for which only coordinates were known. Observations were made with the 76-cm telescope of the South African Astronomical Observatory using an SBIG CCD ST-10XME. The inferred periods and light-curves confirm that CL Eri (P=0.644d), which was found to exhibit the Blazhko effect, and CN Eri (P=0.580d) are RR Lyr-type variables. CM Eri is most probably a Population-Il Cepheid with a period of 0.824d.
