- ID:
- ivo://CDS.VizieR/J/A+AS/111/275
- Title:
- BVRI CCD photometry of NGC 5460
- Short Name:
- J/A+AS/111/275
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present CCD photometry on the BV(RI)_KC_ (Cape) photometric system of the core of the young open cluster, NGC 5460, to a magnitude limit V=~19, R=~19.5. We give photometry for 353 stars and identify 25 as cluster members along with a further 27 as possible members based on their positions in individual colour-magnitude diagrams. We estimate the reddening to the cluster and redefine its distance and age. Four stars are identified as possible variables and their nature discussed.
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- ID:
- ivo://CDS.VizieR/J/AJ/107/230
- Title:
- BVRI CCD photometry of NGC 1904
- Short Name:
- J/AJ/107/230
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present BVRI photometry of three overlapping fields in the globular cluster NGC 1904 (M79), observed with a CCD camera and the 2.2m Max-Planck-Institute telescope at ESO/La Silla. We critically compare our photometry using the INVENTORY data reduction code with results derived by other investigators using different codes. These comparisons convince us that all modern codes give results reliable to at least +/-0.3mag at all levels, as long as the fields are not overly crowded. Specifically, our results for NGC 1904 (M79) are as follows: V(TO)=19.60+/-0.10 (estimated external error), with turnoff colors at B-V=0.40, V-R=0.27, V-I=0.57, and B-I=0.97, all with estimated external errors of +/-0.06. By fitting the four resulting ridge lines to the theoretical isochrones of VandenBerg & Bell [ApJS, 58, 561 (1985)] interpolated to [Fe/H]=-1.60, Y=0.20, and [O/Fe]=0.00, we derive an average value for the age of 16Gyr, where we have adopted E(B-V)=0.01.
- ID:
- ivo://CDS.VizieR/J/A+A/376/144
- Title:
- BV(RI)_C_H{alpha} photometry of NGC 663
- Short Name:
- J/A+A/376/144
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present new BV(RI)_C_H{alpha} photometry of the young open cluster NGC 663. The H{alpha} photometry is complete down to magnitude R_C_=15.4, corresponding to spectral type A5 for the cluster members. This allows detection of mild and strong H{alpha} emission in all B-type stars in the cluster. In addition to the 22 Be stars known in the observed field of NGC 663, we discovered four new faint stars of this type. We find that Be stars in NGC 663 cover the whole range of the B spectral type. They are, however, most populous among stars with spectral types falling in the range between B0 and B3, where their fraction amounts to 31+/-8%. Among B-type stars later than B3, Be stars are much less abundant: only 7 out of 101 observed stars, that is, 7+/-3%, were detected. About 70% of the observed Be stars in NGC 663 show detectable variations of light. In the time interval covered by our observations, the ranges of the largest variations reach 0.4mag in the I_C_ band. By means of the isochrone fitting, we derived the cluster distance of 2.1kpc, age of 20-25Myr, and the mean colour excess E(R-I)_C_=0.54mag, with a ~0.1mag scatter due to differential reddening.
- ID:
- ivo://CDS.VizieR/J/AJ/123/304
- Title:
- BV(RI)_C_JHK H{alpha} photometry in IC 5146
- Short Name:
- J/AJ/123/304
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The B0V star BD+46 3474 lies near the front surface of a dense molecular cloud and illuminates the emission/reflection nebula IC 5146. The HAeBe variable BD +46 3471 is embedded in the same cloud, about 10' (3.5pc) away. CCD photometry in BV(RI)_C_ (to V=22) and in JHK (to about K=16.5) has been obtained for the young clusters surrounding each of these two bright stars. Some 100 emission-H{alpha} stars brighter than R=20.5 have been found in the area, most of them in IC 5146. (Among these are two that have spectra resembling a high-excitation Herbig-Haro [HH] object plus a stellar continuum).
- ID:
- ivo://CDS.VizieR/J/PAZh/30/243
- Title:
- BV(RI)c-JHK photometry of BL Lac in 1999-2001
- Short Name:
- J/PAZh/30/243
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Results of multicolor observations of BL Lac in 1999-2001 are presented. We show that the spectral energy distribution of the variable component in the range from K to B had remained unchanged for three years.
- ID:
- ivo://CDS.VizieR/J/MNRAS/386/521
- Title:
- BV(RI)c light curves of BS Com
- Short Name:
- J/MNRAS/386/521
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We derive the basic physical parameters of the field double-mode RR Lyrae star BS Com from its observed periods and the requirement of consistency between the pulsational and evolutionary constraints. We performed a standard frequency analysis on the V data by discrete Fourier transformation. We derived P0=0.48791d and P1=0.36307d for the periods of the fundamental and the first overtone modes, respectively.
- ID:
- ivo://CDS.VizieR/J/AJ/152/219
- Title:
- BV(RI)c light curves of DD Indi
- Short Name:
- J/AJ/152/219
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Observations and a 2015 Wilson-Devinney Program analysis are undertaken for the first precision observations of DD Indi. DD Indi is of solar-type (T_1_~5750K) and was determined to be a shallow-contact eclipsing binary. It was observed from 2013 June through September at Cerro Tololo InterAmerican Observatory in remote mode. The 24 inch Boller and Chivens reflector, now under management by The Southeastern Association for Resarch in Astronomy (SARA) was used. Five new eclipse timings were obtained, for three primary and two secondary eclipses. Seven more eclipse timings were calculated from All Sky Automated Survey data. A possibly increasing period was found from all available eclipse timings with a 5+/-2x10^-11^xE^2^ quadratic term. A BVR_c_I_c_ simultaneous synthetic light-curve analysis reveals that the system has a mass ratio of ~0.46, a ~140K component temperature difference, and two weak cool spots. The Roche Lobe fill-out of this W-type binary is only ~11%, and an inclination of ~86{deg} was determined. A time of constant light of ~16 minutes is measured around phase zero. More detail is included in this report.
- ID:
- ivo://CDS.VizieR/J/AJ/152/199
- Title:
- BV(RI)c light curves of FF Vul
- Short Name:
- J/AJ/152/199
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- High-precision BVR_c_I_c_ light curves of FF Vul were taken during the fall of 2015 with the Dark Sky Observatory 0.81m reflector of Appalachian State University, and the SARA north 0.91m reflector at KPNO. FF Vul is an eclipsing binary with a period of 0.44 day. A Wilson-Devinney solution shows that the binary is a near-contact, semidetached binary, i.e., with a V1010 Oph-type configuration. Five eclipse timings (three primary and two secondary) were calculated. A quadratic ephemeris was determined indicating that the period is decreasing. A near-equatorial hot spot was modeled on the cooler, secondary star, possibly caused by matter impacting from the primary component via the inner Lagrangian point. The component temperature difference is more than 1500K. The solution confirms a total secondary eclipse of 23 minutes duration. As expected in binaries of this type, there is a magnetic spot region.
- ID:
- ivo://CDS.VizieR/J/AJ/152/227
- Title:
- BV(RI)c light curves of NSVS 5066754
- Short Name:
- J/AJ/152/227
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- BVR_c_I_c_ light curves of NSVS 5066754 were taken on 2014 May at Dark Sky Observatory in North Carolina. This variable is a solar-type eclipsing binary (T1~5750K) with a period of only 0.3751689(1) days. It appeared to be one of the shortest periods in Shaw's list of near-contact binaries. The Binary Maker fits and our Wilson-Devinney solutions show that the binary could have both semidetached and marginal contact binary configurations. Five new times of minimum light were calculated, along with two minima determined from archived All Sky Automated Survey observations. From these minima and the discovery epoch, a quadratic ephemeris was determined. Thus, a magnetic braking scenario is possible. Both semidetached and contact models were explored. A marginal contact solution had the best sum of square residuals. It gave a mass ratio of ~0.5, and a component temperature difference of ~360K, albeit somewhat large for a contact binary. Two substantial cool spots were determined in this solution with 37{deg} and 28{deg} radii and t-factors or 0.94 and 0.78 respectively. The fill-out is very shallow, ~106%. It may have recently achieved contact.
- ID:
- ivo://CDS.VizieR/J/AJ/145/14
- Title:
- BV(RI)c light curves of V1043 Cas
- Short Name:
- J/AJ/145/14
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Complete Bessel BVR_c_I_c_ light curves of V1043 Cassiopeia [2MASS J00371195+5301324, Mis V1292, USNO-A2.0 1425-00875743, {alpha}(2000)=00^h^37^m^11.95^s^, {delta}(2000)=+53{deg}01'32.5"] are analyzed. The system is a member of the small group of pre-contact W UMa binaries (PCWBs). Its light curve has the appearance of an Algol (EA) light curve, however it is made up of dwarf solar type components in a detached mode with a period of only 0.6616days. The analysis includes a period study, an improved ephemeris, a mass ratio search, and a simultaneous BVR_c_I_c_ Wilson-Devinney solution. We document about 20 other PCWBs given in the literature. Several have RS CVn-like properties.
