- ID:
- ivo://CDS.VizieR/J/AJ/145/99
- Title:
- BVRI light curves of SN 2003ie
- Short Name:
- J/AJ/145/99
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present new photometric observations of supernova (SN) 2003ie starting one month before discovery, obtained serendipitously while observing its host galaxy. With only a weak upper limit derived on the mass of its progenitor (<25M_{sun}_) from previous pre-explosion studies, this event could be a potential exception to the "red supergiant (RSG) problem" (the lack of high-mass RSGs exploding as Type IIP SNe). However, this is true only if SN2003ie was a Type IIP event, something which has never been determined. Using recently derived core-collapse SN light-curve templates, as well as by comparison to other known SNe, we find that SN2003ie was indeed a likely Type IIP event. However, with a plateau magnitude of ~-15.5mag, it is found to be a member of the faint Type IIP class. Previous members of this class have been shown to arise from relatively low-mass progenitors (<12M_{sun}_). It therefore seems unlikely that this SN had a massive RSG progenitor. The use of core-collapse SN light-curve templates is shown to be helpful in classifying SNe with sparse coverage. These templates are likely to become more robust as large homogeneous samples of core-collapse events are collected.
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- ID:
- ivo://CDS.VizieR/J/MNRAS/383/1485
- Title:
- BVRI light curves of SN 2003jd
- Short Name:
- J/MNRAS/383/1485
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The results of a worldwide coordinated observational campaign on the broad-lined Type Ic supernova (SN Ic) 2003jd are presented. In total, 74 photometric data points and 26 spectra were collected using 11 different telescopes. SN 2003jd is one of the most luminous SN Ic ever observed. A comparison with other Type Ic supernovae (SNe Ic) confirms that SN 2003jd represents an intermediate case between broad-line events (2002ap, 2006aj) and highly energetic SNe (1997ef, 1998bw, 2003dh, 2003lw), with an ejected mass of M_ej_=3.0+/-1M_{sun}_ and a kinetic energy of E_k_(tot)=7^+3^_-2_x10^51^erg. SN 2003jd is similar to SN 1998bw in terms of overall luminosity, but it is closer to SNe 2006aj and 2002ap in terms of light-curve shape and spectral evolution. The comparison with other SNe Ic suggests that the V-band light curves of SNe Ic can be partially homogenized by introducing a time-stretch factor. Finally, because of the similarity of SN 2003jd to the SN 2006aj/XRF 060218 event, we discuss the possible connection of SN 2003jd with a gamma-ray burst (GRB).
- ID:
- ivo://CDS.VizieR/J/AJ/157/3
- Title:
- BVRI light curves of the binary QS Vir
- Short Name:
- J/AJ/157/3
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We observed the post-common-envelope eclipsing binary with a white dwarf component, QS Vir, using the 1.88 m telescope of Kotammia Observatory in Egypt. The new observations were analyzed together with all multicolor light curves available online (sampling a period of 25 yr), using a full-feature binary system modeling software based on Roche geometry. This is the first time complete photometric modeling was done with most of these data. QS Vir is a detached system, with the red dwarf component underfilling its Roche lobe by a small margin. All light curves feature out-of-eclipse variability that is associated with ellipsoidal variation, mutual irradiation and irregularities in surface brightness of the tidally distorted and magnetically active red dwarf. We tested models with one, two, and three dark spots and found that one spot is sufficient to account for the light curve asymmetry in all data sets, although this does not rule out the presence of multiple spots. We also found that a single spotted model cannot fit light curves observed simultaneously in different filters. Instead, each filter requires a different spot configuration. To thoroughly explore the parameter space of spot locations, we devised a grid-search procedure and used it to find consistent solutions. Based on this, we conclude that the dark spot responsible for light curve distortions has been stable for the past 15 yr, after a major migration that happened between 1993 and 2002, possibly due to a flip-flop event.
- ID:
- ivo://CDS.VizieR/J/ApJ/849/161
- Title:
- BVRI light curves of the BL Lac object Mrk 501
- Short Name:
- J/ApJ/849/161
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present our observations of the optical intra-day variability (IDV) in {gamma}-ray BL Lac object Mrk 501. The observations were run with the 1.02m and 2.4m optical telescopes at Yunnan Observatories from 2005 April to 2012 May. The light curve at the R band on 2010 May 15 passes both variability tests (the F-test and the ANOVA test). A flare within the light curve on 2010 May 15 has a magnitude change of {Delta}m=0.03+/-0.005_stat_+/-0.007_sys_mag, a darkening timescale of {tau}_d_=26.7min., and an amplitude of IDV Amp=2.9%+/-0.7% . A decline described by 11 consecutive flux measurements within the flare can be fitted linearly with a Pearson's correlation coefficient r=0.945 at the confidence level of >99.99% . Under the assumptions that the IDV is tightly connected to the mass of the black hole, and that the flare duration, being two times {tau}_d_, is representative of the minimum characteristic timescale, we can derive upper bounds to the mass of the black hole. In the case of the Kerr black hole, the timescale of {Delta}t_min_^ob^=0.89hr gives M_{bullet}_<~10^9.20^M_{sun}_, which is consistent with measurements reported in the literature. This agreement indicates that the hypothesis about M_{bullet}_ and {Delta}t_min_^ob^ is consistent with the measurements/data.
- ID:
- ivo://CDS.VizieR/J/AJ/145/9
- Title:
- BVRI light curves of the early-type binary V382 Cyg
- Short Name:
- J/AJ/145/9
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We analyze photometric and spectroscopic data and study the orbital period of the early-type interacting binary system V382 Cyg by using all the available data. We obtain a simultaneous light and radial velocity curve solution. The derived physical parameters of the primary and secondary stellar components are M_1_=27.9(5)M_{sun}_, M_2_=20.8(4)M_{sun}_, R_1_=9.7(2)R_{sun}_, R_2_=8.5(2)R_{sun}_, log(L_1_/L_{sun}_)=5.152(20), and log(L_2_/L_{sun}_)=4.954(19) while the separation of the components is a=23.4R_{sun}_. Newly obtained parameters yield the distance of the system to be 1466(76)pc. Analyses of the mid-eclipse times indicate a period increase of dP/dt=4.2(1)x10^-7^days/yr that can be interpreted in terms of the high-mass transfer (dM/dt=6.1(5)x10^-6^M_{sun}_/yr) from the less massive component to the more massive component. Finally, we model the evolution of the components using non-conservative codes and discuss the results obtained. The age of the binary system is estimated to be 3.85Myr.
- ID:
- ivo://CDS.VizieR/J/MNRAS/442/844
- Title:
- BVRI light curves of type II-P supernovae
- Short Name:
- J/MNRAS/442/844
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We study a sample of 23 Type II plateau supernovae (SNe II-P), all observed with the same set of instruments. Analysis of their photometric evolution confirms that their typical plateau duration is 100 d with little scatter, showing a tendency to get shorter for more energetic SNe. We examine the claimed correlation between the luminosity and the rise time from explosion to plateau. We analyse their spectra, measuring typical ejecta velocities, and confirm that they follow a well-behaved power-law decline. We find indications of high-velocity material in the spectra of six of our SNe. We test different dust-extinction correction methods by asking the following - does the uniformity of the sample increase after the application of a given method? A reasonably behaved underlying distribution should become tighter after correction. No method we tested made a significant improvement.
- ID:
- ivo://CDS.VizieR/J/AJ/133/2696
- Title:
- BVRI light curves of Westerlund 1 stars
- Short Name:
- J/AJ/133/2696
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This paper presents the first optical variability study of the Westerlund 1 super star cluster in search of massive eclipsing binary systems. A total of 129 new variable stars have been identified, including the discovery of 4 eclipsing binaries that are cluster members, 1 additional candidate, 8 field binaries, 19 field delta Scuti stars, 3 field W UMa eclipsing binaries, 13 other periodic variables, and 81 long-period or nonperiodic variables. These include the known luminous blue variable, the B[e] star, 11 Wolf-Rayet stars, several supergiants, and other reddened stars that are likely members of Westerlund 1. The bright X-ray source corresponding to the Wolf-Rayet star WR 77o (B) is found to be a 3.51 day eclipsing binary. The discovery of a reddened detached eclipsing binary system implies the first identification of main-sequence stars in Westerlund 1.
- ID:
- ivo://CDS.VizieR/J/AJ/149/48
- Title:
- BVRI light curves of ZZ Eri
- Short Name:
- J/AJ/149/48
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Complete Bessel BVRI light curves of ZZ Eri [2MASSJ04130109-1044545, HV 6280, NSVS 14888164; IRCS position 04:13:01.10-10:44:54.5; V=13.9-14.4-15.0] are observed and analyzed. The system is a southern pre-contact W UMa binary. Its light curve has the appearance of an Algol (EA) light curve, however, it is made up of dwarf solar-type components with a period of only 0.4521days. Our 34year period study yields a sinusoidal fit or an increasing quadratic fit. The sinusoid may indicate that a third body is orbiting the close binary. The lower-limit mass of the third body is near that of the brown dwarf limit (0.095M_{sun}_). Also included is an improved ephemeris, a mass ratio search, and a simultaneous BVRI Wilson-Devinney solution.
- ID:
- ivo://CDS.VizieR/J/ApJS/218/18
- Title:
- 2004-2012 BVRI observations of blazar S5 0716+714
- Short Name:
- J/ApJS/218/18
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present long-term optical multi-band photometric monitoring of blazar S5 0716+714, from 2004 January 11 to 2012 November 4, with high temporal resolution of approximately 15 minutes in the BVRI bands. The source was in an active state during the whole monitoring campaign, showing intraday variability in 11 of 72 days. The average magnitudes in each band were B=14.398, V=13.821, R=13.255, and I=12.885. The overall variability amplitudes were {Delta}B=1^m^.834, , {Delta}V=2^m^.167, {Delta}R=2^m^.148, and {Delta}I=1^m^.912. The structure function showed that typical timescales for intraday variability were between approximately 2 and 7.5hr. The intraday variability amplitudes were from a few percent to approximately 30%. We found typical variation rates of approximately 0.05 mag/hr in both the rising and falling phases, with a minimal variability timescale of 130 minutes. A 10 day period short-term variability was observed simultaneously in the BVRI bands. The discrete correlation function suggests that there is significant correlated variability between the B- and I-band light curves. However, no significant time lags were detected. The spectral behaviors in the different variability episodes were studied, and our observations show bluer-when-brighter behavior on long, short, and intraday timescales for the blazar S5 0716+714. The variability and relevant spectral trends can be explained by the shock-in-jet scenario.
- ID:
- ivo://CDS.VizieR/J/AJ/155/31
- Title:
- 2005-2012 BVRI observations of blazar S5 0716+714
- Short Name:
- J/AJ/155/31
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In order to search for the evidence of quasi-periodic oscillation (QPO) in blazars, multicolor optical observations of the BL Lacertae object S5 0716+714 were performed from 2005 to 2012. For I band observations on 2010 March 19 with low variability amplitude and low flux level, the same QPO~50 minutes at the 99% significance level is confirmed by the ZDCF method, Lomb-Scargle method, REDFIT, and fitting sinusoidal curves. The observed QPO is likely to be explained by accretion disk variability. If the observed QPO indicates an innermost stable orbital period from the accretion disk, the QPO~50 minutes corresponds to a black hole mass of 5.03x10^6^ M_{sun}_ for a non-rotating Schwarzschild black hole and 3.2x10^7^ M_{sun}_ for a maximally rotating Kerr black hole.
