- ID:
- ivo://CDS.VizieR/J/A+A/380/347
- Title:
- BVRI photometry of 27 Kuiper Belt Objects
- Short Name:
- J/A+A/380/347
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present visible (BVRI) photometric measurements of 27 Trans-Neptunian objects, obtained with the FORS2 instrument on the ESO/8m Very Large Telescope (Unit 2) from runs during September and November 2000. The objects display a broad and continuous range of colors from neutral-bluish to very red. Most of the objects also have a linear reflectivity spectrum over the VRI range. There is no evidence of a bimodal color distribution as has been previously reported by other groups. Several objects (1994 TB, 1995 SM_55_, 1998 UR_43_, 1999CF_119_ and 2000 OK_67_) show evidence of changing color, and should be investigated further. The object 1995 SM_55_ deserves a more complete study since its neutral-blue colors suggest it could be a good candidate for hosting cometary activity.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/MNRAS/386/1380
- Title:
- BVRI photometry of LMC star clusters
- Short Name:
- J/MNRAS/386/1380
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a CCD photometric and mass function study of nine young Large Magellanic Cloud star clusters, namely NGC 1767, 1994, 2002, 2003, 2006, SL 538, NGC 2011, 2098 and 2136. BVRI data, reaching down to V~21mag, were collected from the 3.5-m NTT/EFOSC2 in subarcsec seeing conditions. For NGC 1767, 1994, 2002, 2003, 2011 and 2136, broad-band photometric CCD data are presented for the first time.
- ID:
- ivo://CDS.VizieR/J/AJ/154/81
- Title:
- BVRI photometry of luminous stars in M31 and M33
- Short Name:
- J/AJ/154/81
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the first four years of BVRI photometry from an on-going survey to annually monitor the photometric behavior of evolved luminous stars in M31 and M33. Photometry was measured for 199 stars at multiple epochs, including 9 classic Luminous Blue Variables (LBVs), 22 LBV candidates, 10 post-RGB A/F type hypergiants, and 18 B[e] supergiants. At all epochs, the brightness is measured in the V-band and at least one other band to a precision of 0.04-0.10 mag down to a limiting magnitude of 19.0-19.5. Thirty three stars in our survey exhibit significant variability, including at least two classic LBVs caught in S Doradus-type outbursts. A hyperlinked version of the photometry catalog is at http://go.uis.edu/m31m33photcat
- ID:
- ivo://CDS.VizieR/J/A+AS/142/347
- Title:
- BVRI photometry of NGC 6789
- Short Name:
- J/A+AS/142/347
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this paper we present the results of a detailed B, V, R, I, and H{alpha} study of the isolated nearby blue compact dwarf (BCD) galaxy NGC 6789. The observed galaxy has not yet been resolved into stars up to now. On CCD frames obtained with 6m BTA telescope and 2.5m Nordic telescope the galaxy is well resolved. Its colour-magnitude diagram confirms the two component (core-halo) galaxy morphology, which consists of two stellar populations distinct in structure and colour: an inner high surface-brightness young population within 150pc from the center of the galaxy, and a relatively low surface-brightness intermediate-age population extending out to at least 600pc. The distance to the galaxy, estimated from the tip of the red giant branch (TRGB) is 2.1Mpc which places NGC 6789 close to the Local Group. From the mean colour of the RGB, the mean metal abundance of the halo population is estimated as [Fe/H]=~-1dex.
- ID:
- ivo://CDS.VizieR/J/A+A/345/521
- Title:
- BVRI photometry of NGC 2264
- Short Name:
- J/A+A/345/521
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The pre-main-sequence (PMS) population in the mass range between =~0.2 and =~3M_{sun}_ in southern part of the star-forming region NGC 2264 has been studied, determining both the Initial Mass Function in the region as well as the star-formation rates for different mass ranges. The sample is a composite one, derived through the union of samples obtained through different techniques and each suffering from different biases: previously known PMS stars in the region from the literature, photometrically-selected T Tauri candidates (from our own photometric data, discussed in detail in the present paper) and X-ray selected PMS candidates (discussed in detail in a companion paper) have been joined to form a sample which we show to be statistically complete (i.e. free from the biases which affect each of the parent samples) down to =~0.6M_{sun}_ (while being incomplete at lower masses). Individual masses and ages have been derived by placing the individual stars on evolutionary tracks, allowing us to derive both the IMF and the star formation rate. The Initial Mass Function thus derived for NGC 2264 shows evidence for a bimodal distribution of masses, with a break in the IMF at around 1M_{sun}_.
- ID:
- ivo://CDS.VizieR/J/other/NewA/27.25
- Title:
- BVRI photometry of Nova KT Eri 2009
- Short Name:
- J/other/NewA/27.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We obtained extensive new BVRcIc photometry of Nova KT Eri 2009 over a 539-day interval during the post-outburst quiescence, from 30 September 2011 to 22 March 2013 (days +684 to +1223 past maximum). The median magnitudes we measured are B=15.24, V=15.00, Rc=14.75 and Ic=14.49. A marked variability is present (total amplitude of {Delta}V=1.6mag). Accounting for a generally overlooked correction to blue photographic magnitudes calibrated against modern B-band data, we found that mean brightness and amplitude of variability of KT Eri in quiescence are the same before and after the 2009 nova outburst. The distance to KT Eri derived from standard relations involving the absolute magnitude at maximum vs rate of decline (MMRD), is ~6.5kpc. At such a distance, to fit the BVRcIc + JHK flux distribution of KT Eri in quiescence requires an 8200K blackbody with a radius of 3.5R_{sun}_, which is vastly larger than the radius of typical accretion disks of CVs and classical old novae (0.1R_{sun}_). The distance to KT Eri could therefore be much shorter than expected from MMRD relation. We also observed a new eclipse-like minimum to occur right on time following the 752 day period suspected to modulate the quiescence of KT Eri before the outburst. The nature of this period remains unclear. The faintness of KT Eri at infrared wavelengths (K=14.1) precludes it from being the orbital period of the accreting WD, because in such a case the Roche lobe filling companion would be a cool giant shining at K~9mag.
- ID:
- ivo://CDS.VizieR/J/other/PZ/30.4
- Title:
- BVRI photometry of nova V445 Pup
- Short Name:
- J/other/PZ/30.4
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- V445 Pup was a peculiar nova having no hydrogen spectral lines in the outburst. The spectrum contained strong emission lines of carbon, oxygen, calcium, sodium and iron. We have performed digital processing of photographic images of the V445 Pup progenitor using astronomical plate archives. The brightness of the progenitor in the B band was 14.3mag. It was found to be a periodic variable star, its most probable period being 0d.650654+/-0.000011d. The light curve shape suggests that the progenitor was a common-envelope binary having a spot on the surface and variable surface brightness. The spectral energy distribution of the progenitor between 0.44 and 2.2um was similar to that of an A0V type star.
- ID:
- ivo://CDS.VizieR/J/A+AS/129/569
- Title:
- BVRI photometry of OJ 287
- Short Name:
- J/A+AS/129/569
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Results of BVRI CCD photometric monitoring and fast photometry in the I band for the blazar OJ 287 in 1994-1995 are presented. The predicted outburst of the blazar had been observed, the maximum appeared in 1994 November, after that, the luminosity decreased by 1.6mag for about three months and dropped to near the level in 1994 April. Rapid variations with timescales of minutes, hours and one day were observed in our observations, with small amplitude. The amplitude of the most rapid variations (minutes) is in the range of 0.043-0.12mag . The results of the statistical analysis of the fast photometry data are as follows. In five nights out of six rapid variability appeared in the sampling interval, which ranged from 3.4 minutes to 6.5 minutes, with a rms amplitude of flux variations of 1.70%-2.3%. The rapid variability can be explained by the model of shocks within turbulent jet or of vortices and magnetic flux tubes on accretion disk.
- ID:
- ivo://CDS.VizieR/J/PASP/106/828
- Title:
- BVRI photometry of Omega Cen
- Short Name:
- J/PASP/106/828
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- BVRI photometry is given for stars in the omega Centauri (= NGC 5139 = C 1323-472) calibration field for the Wide Field/Planetary Camera of the Hubble Space Telescope.
- ID:
- ivo://CDS.VizieR/J/AN/326/3
- Title:
- BVRI photometry of 4 open clusters
- Short Name:
- J/AN/326/3
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- CCD photometry of the galactic open clusters NGC 2627, NGC 5617, Pismis 7, and Ruprecht 75 is presented. For the first cluster, BV data are given, for the others the data are BV(RI)_c. The star coordinates are relative to the corresponding cluster center. The observations were carried out from the Complejo Astronomico El Leoncito (Argentina), and from Las Campanas (Chile). Each cluster was observed on two different nights; when possible, measurements for a given star were averaged. NGC 2627 observations were carried out from CASLEO on the nights of 7-8 January 1997 and 23-24 April 2001, in the BV filters. NGC 5617 data in the BVRI filters were obtained at Las Campanas on the nights 10-11 and 11-12 April 1996, and at CASLEO on the 1-2 April 2001 night. Pismis 7 was observed from Campanas on the 13-14 and 15-16 April 1996 nights (BVRI). Ruprecht 75 data in the BVRI filters were obtained at Las Campanas on the 12-13 April 1996 night, and at CASLEO on the 20-21 April 2001 night.
