- ID:
- ivo://CDS.VizieR/J/A+A/497/481
- Title:
- UBV(RI)c time series of V372 Ser
- Short Name:
- J/A+A/497/481
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The first UBV(RI)_C time series photometry of the RRd star V372 Ser is presented to determine some parameters of the star. In April, May 2007 2812 U, B, V, R_C, I_C frames were obtained at Konkoly and Teide Observatories, 1508 V observations were collected from the literature. Fourier fitted light curves have been derived in all bands. The non-linearly coupled frequencies f_0=(2.121840+/-.000001)c/day, f_1_=(2.851188+/-.000001)c/d, i.e. periods P_0_=0.4712891+/-.0000002days, P_1_=0.3507310+/-.0000001d, P_1_/P_0_=0.7441950, amplitudes A_0_(V)=0.15399mag, A_1_(V)=0.20591mag, and phases have been found. A_1_/A_0_=1.319+/-.008 has been found from averaging the amplitude ratio in the different bands i.e. the first overtone is the dominant pulsation mode. From the V observations upper limits are given for secular change of the Fourier parameters. The period ratio and period put V372 Ser among the RRd stars of the globular clusters M3 and IC 4499, mass, luminosity, and metallicity estimates are given.
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Search Results
- ID:
- ivo://CDS.VizieR/J/MNRAS/466/392
- Title:
- UBVRICT1T2 photometry of 7 open clusters
- Short Name:
- J/MNRAS/466/392
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a comprehensive UBVRI and Washington CT_1_T_2_ photometric analysis of seven catalogued open clusters, namely: Ruprecht 3, 9, 37, 74, 150, ESO 324-15 and 436-2. The multiband photometric data sets in combination with 2MASS photometry and Gaia astrometry for the brighter stars were used to estimate their structural parameters and fundamental astrophysical properties. We found that Ruprecht 3 and ESO 436-2 do not show self-consistent evidence of being physical systems. The remained studied objects are open clusters of intermediate age (9.0<=log(t[yr^-1^])<=9.6), of relatively small size (r_cls_~0.4-1.3pc) and placed between 0.6 and 2.9kpc from the Sun. We analysed the relationships between core, half-mass, tidal and Jacoby radii as well as half-mass relaxation times to conclude that the studied clusters are in an evolved dynamical stage. The total cluster masses obtained by summing those of the observed cluster stars resulted to be ~10-15 per cent of the masses of open clusters of similar age located closer than 2kpc from the Sun. We found that cluster stars occupy volumes as large as those for tidally filled clusters.
- ID:
- ivo://CDS.VizieR/J/PASJ/59/955
- Title:
- UBVRI differential photometry of BH Vir
- Short Name:
- J/PASJ/59/955
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Photoelectric light curves of BH Vir in the UBVRI bands observed by Arevalo et al. (1987IBVS.3117....1A, 1990ApJ...354..352Z) in 1986 were analyzed by using the latest version of the Wilson-Devinney program and to investigate the photometric parameters and spot activity. Satisfactory fits were obtained by assuming a hot spot only on the secondary star.
- ID:
- ivo://CDS.VizieR/J/MNRAS/394/872
- Title:
- UBVRI differential photometry of DM UMa
- Short Name:
- J/MNRAS/394/872
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present extensive UBVRI photometry of the active RS CVn binary DM UMa obtained at two different observatories over 1988-2008.
- ID:
- ivo://CDS.VizieR/J/AJ/132/1153
- Title:
- UBV(RI) differential photometry of FI Boo
- Short Name:
- J/AJ/132/1153
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- UBVR_C_I_C_ photometry of the W UMa eclipsing binary FI Bootis has been obtained and analyzed simultaneously with previously published photometry and radial velocities. The analysis of the light and radial velocity curves shows that the system is an A-type W UMa system consisting of stars with masses 0.82 and 0.31M_{sun}_.
- ID:
- ivo://CDS.VizieR/J/A+A/441/905
- Title:
- UBVRI from the Garching-Bonn Deep Survey
- Short Name:
- J/A+A/441/905
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present first results of our search for high-redshift galaxies in deep CCD mosaic images. As a pilot study for a larger survey, very deep images of the Chandra Deep Field South (CDFS), taken with WFI@MPG/ESO2.2m, are used to select large samples of 1070 U-band and 565 B-band dropouts with the Lyman-break method.
- ID:
- ivo://CDS.VizieR/J/MNRAS/433/1871
- Title:
- UBVRI griz light curves of SN 2012aw
- Short Name:
- J/MNRAS/433/1871
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present densely sampled UBVRI/griz photometric and low-resolution (6-10{AA}) optical spectroscopic observations from 4 to 270d after explosion of a newly discovered Type II SN 2012aw in a nearby (~9.9Mpc) galaxy M95. The light-curve characteristics of apparent magnitudes, colours, bolometric luminosity and the presence and evolution of prominent spectral features are found to have striking similarity with the archetypal IIP SNe 1999em, 1999gi and 2004et. The early time observations of SN 2012aw clearly detect minima in the light curve of V, R and I bands near 37d after explosion and this we suggest to be an observational evidence for emergence of recombination phase. The mid-plateau M_V_ magnitude (-16.67+/-0.04) lies in between the bright (~-18) and subluminous (~-15) IIP SNe. The mass of nickel is 0.06+/-0.01M{sun}. The synow modelling of spectra indicate that the value and evolution of the photospheric velocity is similar to SN 2004et, but about ~600km/s higher than that of SNe 1999em and 1999gi at comparable epochs. This trend is more apparent in the line velocities of H{alpha} and H{beta}. A comparison of ejecta velocity properties with that of existing radiation-hydrodynamical simulations indicate that the energy of explosion lies in the range 1-2x10^51^ergs; a further comparison of nebular phase [OI] doublet luminosity with SNe 2004et and 1987A indicate that the mass of progenitor star is about 14 to 15M_{sun}_. The presence of high-velocity absorption features in the mid-to-late plateau and possibly in early phase spectra show signs of interaction between ejecta and the circumstellar matter; being consistent with its early time detection at X-ray and radio wavebands.
- ID:
- ivo://CDS.VizieR/J/other/NewA/15.108
- Title:
- UBVRIH{alpha} of {eta} Car in 2009
- Short Name:
- J/other/NewA/15.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The periodic events occurring in {eta} Carinae have been widely monitored during the last three 5.5-year cycles. The last one recently occurred in January 2009 and more exhaustive observations have been made at different wavelength ranges. If these events are produced when the binary components approach periastron, the timing and sampling of the photometric features can provide more information about the geometry and physics of the system. Thus, we continued with our ground-based optical photometric campaign started in 2003 to record the behaviour of the 2009.0 event in detail. This time the observation program included a new telescope to obtain information from other photometric bands. The daily monitoring consists of the acquisition of CCD images through standard UBVRI filters and a narrow H{alpha} passband. The subsequent differential photometry includes the central region of the object and the whole Homunculus nebula. The results of our relative UBVRIH{alpha} photometry, performed from November 2008 up to the end of March 2009, are presented in this work, which comprises the totality of the event. The initial rising branch, the maximum, the dip to the minimum and the recovering rising phase strongly resemble a kind of eclipse. All these features happened on time - according to that predicted - although there are some photometric differences in comparison with the previous event. We made a new determination of 2022.8 days for the period value using the present and previous "eclipse-like" event data. These results strongly support the binarity hypothesis for {eta} Car. In this paper, the complete dataset with the photometry of the 2009.0 event is provided to make it readily available for further analysis.
- ID:
- ivo://CDS.VizieR/J/A+A/511/A25
- Title:
- UBVRIH{alpha} photometry of NGC6383
- Short Name:
- J/A+A/511/A25
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The very young open cluster NGC 6383 centered on the O-star binary HD 159176 is an interesting place for studying the impact of early-type stars with strong radiation fields and powerful winds on the formation processes of low-mass stars. To investigate this process, it is necessary to determine the characteristics (age, presence, or absence of circumstellar material) of the population of low-mass pre-main-sequence (PMS) stars in the cluster. We obtained deep U B V Rc Ic H{alpha} photometric data of the entire cluster as well as medium-resolution optical spectroscopy of a subsample of X-ray selected objects. Our spectroscopic data reveal only very weak H{alpha} emission lines in a few X-ray selected PMS candidates. We photometrically identify a number of H-{alpha} emission candidates but their cluster membership is uncertain. We find that the fainter objects in the field of view have a wide range of extinction (up to A_V_=20), one X-ray selected OB star having A_V_~8. Our investigation uncovers a population of PMS stars in NGC 6383 that are probably coeval with HD 159176. In addition, we detect a population of reddened objects that are probably located at different depths within the natal molecular cloud of the cluster. Finally, we identify a rather complex spatial distribution of H{alpha} emitters, which is probably indicative of a severe contamination by foreground and background stars.
- ID:
- ivo://CDS.VizieR/J/A+A/402/549
- Title:
- UBVRIHalpha photometry of NGC 3293
- Short Name:
- J/A+A/402/549
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Deep and extensive CCD photometric observations at UBV(RI)cH{alpha} were carried out in the area of the open cluster NGC 3293. The new data set allows to see the entire cluster sequence down to Mv~+4.5, revealing that stars with Mv<-2 are evolving off the main sequence; stars with -2<Mv<+2 are located on the main sequence and stars with Mv>+2 are placed above it. According to our analysis, the cluster distance is d=2750+/-250pc (V0-Mv=12.2+/-0.2) and its nuclear age is 8+/-1Myr. NGC 3293 contains an important fraction of pre-main sequence (PMS) stars distributed along a parallel band to the ZAMS with masses from 1 to 2.5M_{sun}_ and a mean contraction age of 10Myr. This last value does not differ too much from the nuclear age estimate. If we take into account the many factors that may affect the PMS star positions on the colour-magnitude diagram, both ages can be perfectly reconciled. The star formation rate, on the other hand, suggests that NGC 3293 stars formed surely in one single event, therefore favouring a coeval process of star formation. Using the Halpha data, we detected nineteen stars with signs of Halpha emission in the region of NGC 3293, another indication that the star formation process is still active in the region. The computed initial mass function for the cluster has a slope of x=1.2+/-0.2, a bit flatter than the typical slope for field stars and similar to the values found for other young open clusters.
