- ID:
- ivo://CDS.VizieR/J/AcA/63/1
- Title:
- OGLE-IV Magellanic Bridge Data supernovae
- Short Name:
- J/AcA/63/1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We analyze two years (mid-2010 to mid-2012) of OGLE-IV data covering ~65deg^2^ of the Magellanic Bridge (the area between the Magellanic Clouds) and find 130 transient events including 126 supernovae (SNe), two foreground dwarf novae and another two SNe-like transients that turned out to be active galactic nuclei (AGNs). We show our SNe detection efficiency as a function of SN peak magnitude based on available SNe rate estimates. It is 100% for SNe peak magnitudes I<18.8mag and drops to 50% at I~19.7mag. With our current observing area between and around the Magellanic Clouds (~600deg^2^), we expect to find 24 SNe peaking above I<18mag, 100 above I<19mag, and 340 above I<20mag, annually. We briefly introduce our on-line near-real-time detection system for SNe and other transients, the OGLE Transient Detection System.
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- ID:
- ivo://CDS.VizieR/J/AcA/64/197
- Title:
- OGLE-IV 2012-2014 transients
- Short Name:
- J/AcA/64/197
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the design and first results of a real-time search for transients within the 650 sq. deg. area around the Magellanic Clouds, conducted as part of the OGLE-IV project and aimed at detecting supernovae, novae and other events. The average sampling of about four days from September to May, yielded a detection of 238 transients in 2012/2013 and 2013/2014 seasons. The superb photometric and astrometric quality of the OGLE data allows for numerous applications of the discovered transients. We use this sample to prepare and train a Machine Learning-based automated classifier for early light curves, which distinguishes major classes of transients with more than 80% of correct answers. Spectroscopically classified 49 supernovae Type Ia are used to construct a Hubble Diagram with statistical scatter of about 0.3mag and fill the least populated region of the redshifts range in the Union sample. We investigate the influence of host galaxy environments on supernovae statistics and find the mean host extinction of A_I_=0.19+/-0.10mag and A_V_=0.39+/-0.21mag based on a subsample of supernovae Type Ia. We show that the positional accuracy of the survey is of the order of 0.5pixels (0.13") and that the OGLE-IV Transient Detection System is capable of detecting transients within the nuclei of galaxies. We present a few interesting cases of nuclear transients of unknown type. All data on the OGLE transients are made publicly available to the astronomical community via the OGLE website.
- ID:
- ivo://CDS.VizieR/J/ApJS/213/19
- Title:
- Optical and near-IR light curves of 64 SNe
- Short Name:
- J/ApJS/213/19
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a densely sampled, homogeneous set of light curves of 64 low-redshift (z<~0.05) stripped-envelope supernovae (SNe of Type IIb, Ib, Ic, and Ic-BL). These data were obtained between 2001 and 2009 at the Fred L. Whipple Observatory (FLWO) on Mount Hopkins in Arizona, with the optical FLWO 1.2m and the near-infrared (NIR) Peters Automated Infrared 1.3m telescopes. Our data set consists of 4543 optical photometric measurements on 61 SNe, including a combination of UBVRI, UBVr'i', and u'BVr'i', and 1919 JHK_s_ NIR measurements on 25 SNe. This sample constitutes the most extensive multi-color data set of stripped-envelope SNe to date. Our photometry is based on template-subtracted images to eliminate any potential host-galaxy light contamination. This work presents these photometric data, compares them with data in the literature, and estimates basic statistical quantities: date of maximum, color, and photometric properties. We identify promising color trends that may permit the identification of stripped-envelope SN subtypes from their photometry alone. Many of these SNe were observed spectroscopically by the Harvard-Smithsonian Center for Astrophysics (CfA) SN group, and the spectra are presented in a companion paper. A thorough exploration that combines the CfA photometry and spectroscopy of stripped-envelope core-collapse SNe will be presented in a follow-up paper.
- ID:
- ivo://CDS.VizieR/J/ApJ/863/90
- Title:
- Optical and NIR LCs of the nearby SN 2017cbv
- Short Name:
- J/ApJ/863/90
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- On 2017 March 11, the DLT40 Transient Discovery Survey discovered SN2017cbv in NGC 5643, a Type 2 Seyfert Galaxy in the Lupus Constellation. SN 2017cbv went on to become a bright Type Ia supernova, with a Vmax of 11.51+/-0.05mag. We present early time optical and infrared photometry of SN 2017cbv covering the rise and fall of over 68 days. We find that SN 2017cbv has a broad light curve {Delta}m_15_(B)=0.88+/-0.07, a B-band maximum at 2457840.97+/-0.43, a negligible host galaxy reddening where E(B-V)_host_~0, and a distance modulus of 30.49+/-0.32 to the SN, corresponding to a distance of 12.58_-1.71_^+1.98^Mpc. We also present the results of two different numerical models we used for analysis in this paper: SALT2, an empirical model for Type Ia supernova optical light curves that accounts for variability components; and SNooPy, the CSP-II light-curve model that covers both optical and near-infrared wavelengths and is used for distance estimates.
- ID:
- ivo://CDS.VizieR/J/ApJ/904/14
- Title:
- Optical and NIR observation of SN (Ia) 2017cbv
- Short Name:
- J/ApJ/904/14
- Date:
- 24 Mar 2022 06:19:55
- Publisher:
- CDS
- Description:
- Supernova (SN) 2017cbv in NGC5643 is one of a handful of Type Ia supernovae (SNeIa) reported to have excess blue emission at early times. This paper presents extensive BVRIYJHKs-band light curves of SN2017cbv, covering the phase from -16 to +125days relative to B-band maximum light. The SN2017cbv reached a B-band maximum of 11.710{+/-}0.006mag, with a postmaximum magnitude decline of {Delta}m15(B)=0.990{+/-}0.013mag. The SN suffered no host reddening based on Phillips intrinsic color, the Lira-Phillips relation, and the CMAGIC diagram. By employing the CMAGIC distance modulus {mu}=30.58{+/-}0.05mag and assuming H0=72km/s/Mpc, we found that 0.73M{sun} 56Ni was synthesized during the explosion of SN2017cbv, which is consistent with estimates using reddening- and distance-free methods via the phases of the secondary maximum of the near-IR- (NIR-) band light curves. We also present 14 NIR spectra from -18 to +49 days relative to the B-band maximum light, providing constraints on the amount of swept-up hydrogen from the companion star in the context of the single degenerate progenitor scenario. No Pa{beta} emission feature was detected from our postmaximum NIR spectra, placing a hydrogen mass upper limit of 0.1M{sun}. The overall optical/NIR photometric and NIR spectral evolution of SN2017cbv is similar to that of a normal SN Ia, even though its early evolution is marked by a flux excess not seen in most other well-observed normal SNe Ia. We also compare the exquisite light curves of SN2017cbv with some Mch delayed detonation models and sub-Mch double detonation models.
- ID:
- ivo://CDS.VizieR/J/ApJ/895/118
- Title:
- Optical and NIR photometry of 2 Ia type supernovae
- Short Name:
- J/ApJ/895/118
- Date:
- 11 Mar 2022
- Publisher:
- CDS
- Description:
- We present photometric and spectroscopic observations of SN2013aa and SN2017cbv, two nearly identical type Ia supernovae (SNeIa) in the host galaxy NGC5643. The optical photometry has been obtained using the same telescope and instruments used by the Carnegie Supernova Project. This eliminates most instrumental systematics and provides light curves in a stable and well-understood photometric system. Having the same host galaxy also eliminates systematics due to distance and peculiar velocity, providing an opportunity to directly test the relative precision of SNeIa as standard candles. The two SNe have nearly identical decline rates, negligible reddenings, and remarkably similar spectra, and, at a distance of ~20Mpc, they are ideal potential calibrators for the absolute distance using primary indicators such as Cepheid variables. We discuss to what extent these two SNe can be considered twins and compare them with other supernova "siblings" in the literature and their likely progenitor scenarios. Using 12 galaxies that hosted two or more SNe Ia, we find that when using SNeIa, and after accounting for all sources of observational error, one gets consistency in distance to 3%.
- ID:
- ivo://CDS.VizieR/J/ApJ/853/62
- Title:
- Optical and NIR spectra and LCs of SN2016ija
- Short Name:
- J/ApJ/853/62
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present our analysis of the Type II supernova DLT16am (SN2016ija). The object was discovered during the ongoing D<40Mpc (DLT40) one-day cadence supernova search at r~20.1mag in the "edge-on" nearby (D=20.0+/-4.0Mpc) galaxy NGC1532. The subsequent prompt and high-cadenced spectroscopic and photometric follow-up revealed a highly extinguished transient, with E(B-V)=1.95+/-0.15mag, consistent with a standard extinction law with R_V_=3.1 and a bright (M_V_=-18.48+/-0.77mag) absolute peak magnitude. A comparison of the photometric features with those of large samples of SNe II reveals a fast rise for the derived luminosity and a relatively short plateau phase, with a slope of S_50V_=0.84+/-0.04mag/50days, consistent with the photometric properties typical of those of fast-declining SNeII. Despite the large uncertainties on the distance and the extinction in the direction of DLT16am, the measured photospheric expansion velocity and the derived absolute V-band magnitude at ~50days after the explosion match the existing luminosity-velocity relation for SNeII.
- ID:
- ivo://CDS.VizieR/J/A+A/578/A9
- Title:
- Optical and NIR spectra of SN iPTF13ebh
- Short Name:
- J/A+A/578/A9
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2.3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR CI lines, and the CI {lambda}1.0693um line is the strongest ever observed in a SN Ia. Interestingly, no strong optical CII counterparts were found, even though the optical spectroscopic time series began early and is densely-cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR CI compared to the weaker optical CII appears to be general in SNe Ia. iPTF13ebh is a fast decliner with {Delta}m15(B)=1.79+/-0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a "transitional" event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest composition and density of the inner core similar to that of 91bg-like events, and a deep reaching carbon burning layer not observed in slower declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the SiII {lambda}0.6355um line, implying a long dark phase of ~4 days.
- ID:
- ivo://CDS.VizieR/J/AJ/148/1
- Title:
- Optical and ultraviolet photometry of SN 2012fr
- Short Name:
- J/AJ/148/1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Extensive optical and UltraViolet (UV) observations of the type Ia supernova (SN Ia) 2012fr are presented in this paper. It has a relatively high luminosity, with an absolute B-band peak magnitude of about -19.5mag and a smaller post-maximum decline rate than normal SNe Ia (e.g., {Delta}m_15_(B)=0.85+/-0.05mag). Based on the UV and optical light curves, we derived that a ^56^Ni mass of about 0.88M_{sun}_ was synthesized in the explosion. The earlier spectra are characterized by noticeable high-velocity features of Si II {lambda}6355 and Ca II with velocities in the range of ~22000-25000km/s. At around the maximum light, these spectral features are dominated by the photospheric components which are noticeably narrower than normal SNe Ia. The post-maximum velocity of the photosphere remains almost constant at ~12000km/s for about one month, reminiscent of the behavior of some luminous SNe Ia like SN 1991T. We propose that SN 2012fr may represent a subset of the SN 1991T-like SNe Ia viewed in a direction with a clumpy or shell-like structure of ejecta, in terms of a significant level of polarization reported in Maund et al. (2013MNRAS.433L..20M).
- ID:
- ivo://CDS.VizieR/J/AJ/151/125
- Title:
- Optical and UV photometry of SN 2013dy
- Short Name:
- J/AJ/151/125
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Extensive and independent observations of Type Ia supernova (SNIa) SN2013dy are presented, including a larger set of UBVRI photometry and optical spectra from a few days before the peak brightness to ~200days after explosion, and ultraviolet (UV) photometry spanning from t~-10days to t~+15days refers to the B band maximum. The peak brightness (i.e., M_B_=-19.65+/-0.40mag; L_max_=[1.95+/-0.55]*10^43^/ergs) and the mass of synthesized ^56^Ni (i.e., M(^56^Ni)=0.90+/-0.26M_{Sun}_) are calculated, and they conform to the expectation for an SNIa with a slow decline rate (i.e., {Delta}m_15_(B)=0.90+/-0.03mag). However, the near infrared (NIR) brightness of this SN (i.e., M_H_=-17.33+/-0.30mag) is at least 1.0mag fainter than usual. Besides, spectroscopy classification reveals that SN2013dy resides on the border of "core normal" and "shallow silicon" subclasses in the Branch et al. classification scheme, or on the border of the "normal velocity" SNeIa and 91T/99aa-like events in the Wang et al. system. These suggest that SN2013dy is a slow-declining SNIa located on the transitional region of nominal spectroscopic subclasses and might not be a typical normal sample of SNeIa.
