ZTF Early Observations of Type Ia Supernovae. I. Properties of the 2018 Sample

Yao, Yuhan; Miller, A. A.; Kulkarni, S. R.; Bulla, Mattia; Masci, Frank J.; Goldstein, D.; Goobar, A.; Nugent, P.; Dugas, A.; Blagorodnova, N.; Neill, James D.; Rigault, M.; Sollerman, J.; Nordin, J.; Bellm, Eric C.; Cenko, S. Bradley; De, Kishalay; Dhawan, Suhail; Feindt, U.; Fremling, C.; Gatkine, Pradip; Graham, M. J.; Graham, M. L.; Ho, Anna Y. Q.; Hung, T.; Kasliwal, M. M.; Kupfer, Thomas; Laher, Russ R.; Perley, D.; Rusholme, B.; Shupe, D. L.; Soumagnac, Maayane T.; Taggart, K.; Walters, Richard; Yan, Lin

doi:10.3847/1538-4357/ab4cf5

Cited by 99 publications

(162 citation statements)

References 104 publications

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“…Following Yao et al (2019), we perform forced point-spread function (PSF) photometry on ZTF difference images generated with the ZTF real-time reduction and image subtraction pipeline (Masci et al 2019). ZTF image subtraction is based on the Zackay et al (2016) image subtraction method.…”

Section: Optical Photometrymentioning

confidence: 99%

“…Within the ensemble, we use 100 walkers, each of which is run until convergence or 100,000 steps, whichever comes first. The test for convergence follows steps outlined in Yao et al (2019) and Miller et al (2020). We adopt the 68% credible region (i.e., 16th and 84th percentiles of posterior probability distributions) as the model uncertainties quoted in Table B1.…”

Section: B1 Modeling the Physical Evolutionmentioning

confidence: 99%

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SN2019dge: A Helium-rich Ultra-stripped Envelope Supernova

Yao

Kasliwal

et al. 2020

ApJ

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We present observations of ZTF18abfcmjw (SN2019dge), a helium-rich supernova with a fast-evolving light curve indicating an extremely low ejecta mass (≈0.33 M e) and low kinetic energy (≈1.3×10 50 erg). Early-time (<4 days after explosion) photometry reveals evidence of shock cooling from an extended helium-rich envelope of∼0.1 M e located ∼1.2×10 13 cm from the progenitor. Early-time He II line emission and subsequent spectra show signatures of interaction with helium-rich circumstellar material, which extends from5×10 13 cm to2×10 16 cm. We interpret SN2019dge as a helium-rich supernova from an ultra-stripped progenitor, which originates from a close binary system consisting of a mass-losing helium star and a low-mass main-sequence star or a compact object (i.e., a white dwarf, a neutron star, or a black hole). We infer that the local volumetric birth rate of 19dge-like ultra-stripped SNe is in the range of 1400-8200-Gpc yr 3 1 (i.e., 2%-12% of core-collapse supernova rate). This can be compared to the observed coalescence rate of compact neutron star binaries that are not formed by dynamical capture.

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Section: Optical Photometrymentioning

confidence: 99%

Section: B1 Modeling the Physical Evolutionmentioning

confidence: 99%

SN2019dge: A Helium-rich Ultra-stripped Envelope Supernova

Yao

Kasliwal

et al. 2020

ApJ

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“…In Figure 17, we show early (<4 days) light curves of five nearby (z  0.05) Ic-BL SNe observed as part of ZTF's highcadence surveys, which were spectroscopically classified as part of the ZTF flux-limited (Fremling et al 2020) and volume-limited (De et al 2019) experiments. The light curves shown are from forced photometry on P48 images (Yao et al 2019), and epochs of spectroscopy are marked with an "S." For the two most luminous events, we show the light curve of SN 2006aj for comparison. We can rule out a first peak like that of SN 2006aj (duration ≈1 days, peak luminosity ≈−18) for all events except one (ZTF 19ablesob).…”

Section: Early Ztf Light Curves Of Nearby Ic-bl Snementioning

confidence: 99%

“…Early (D  t 4 days) light curves of nearby Ic-BL SNe observed as part of ZTF's high-cadence surveys from forced photometry on P48 images(Yao et al 2019). The B-band light curve of SN 2006aj is shown as a gray line for comparison.…”

mentioning

confidence: 99%

SN 2020bvc: A Broad-line Type Ic Supernova with a Double-peaked Optical Light Curve and a Luminous X-Ray and Radio Counterpart

Kulkarni

Perley

et al. 2020

ApJ

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We present optical, radio, and X-ray observations of SN 2020bvc (=ASASSN-20bs, ZTF 20aalxlis), a nearby (= z 0.0252; d=114 Mpc) broad-line (BL) Type Ic supernova (SN) and the first double-peaked Ic-BL discovered without a gamma-ray burst (GRB) trigger. Our observations show that SN 2020bvc shares several properties in common with the Ic-BL SN 2006aj, which was associated with the low-luminosity gamma-ray burst (LLGRB) 060218. First, the 10 GHz radio luminosity (»-L 10 erg s radio 37 1) is brighter than ordinary core-collapse SNe but fainter than LLGRB SNe such as SN 1998bw (associated with LLGRB 980425). We model our VLA observations (spanning 13-43 days) as synchrotron emission from a mildly relativistic (v  0.3c) forward shock. Second, with Swift and Chandra, we detect X-ray emission (L X ≈10 41 ergs 1) that is not naturally explained as inverse Compton emission or part of the same synchrotron spectrum as the radio emission. Third, high-cadence (6× night-1) data from the Zwicky Transient Facility (ZTF) show a double-peaked optical light curve, the first peak from shock cooling of extended low-mass material (mass <-M M 10 e 2  at radius R e >10 12 cm) and the second peak from the radioactive decay of Ni 56. SN 2020bvc is the first double-peaked Ic-BL SN discovered without a GRB trigger, so it is noteworthy that it shows X-ray and radio emission similar to LLGRB SNe. For four of the five other nearby (z0.05) Ic-BL SNe with ZTF high-cadence data, we rule out a first peak like that seen in SN 2006aj and SN 2020bvc, i.e., that lasts ≈1 dayand reaches a peak luminosity M≈−18. Follow-up X-ray and radio observations of Ic-BL SNe with well-sampled early optical light curves will establish whether double-peaked optical light curves are indeed predictive of LLGRB-like X-ray and radio emission. Unified Astronomy Thesaurus concepts: Radio transient sources (2008); High energy astrophysics (739); Transient sources (1851); Core-collapse supernovae (304); Supernovae (1668); Type Ic supernovae (1730); X-ray transient sources (1852); Gamma-ray bursts (629) Supporting material: data behind figure, machine-readable table

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“…Recently, thanks to a booming number of earlyphase SNe Ia discovered by transient surveys with day or even shorter cadences, it turns out that the fraction of such "long-rising" normal SNe Ia is non-negligible. For instance, by investigating normal SNe Ia with g-band rise times more than 18 days (rest frame, all SNe Ia with observed g-band absolute magnitudes between −19.0 and −19.4) discovered by ZTF (Yao et al 2019), over half (ZTF18abkhcwl, ZTF18aavrwhu, ZTF18abxxssh, ZTF18abpamut, ZTF18aaqqoqs, and ZTF18abimsyv) show possible early excess in their g-band light curves, indicating an extended rise-time distribution of normal SNe Ia and a high early-excess fraction of the "longrising" normal SNe Ia. The long rise times discovered in a fraction of normal SNe Ia suggests that many normal SNe Ia may have dark phases lasting for few days after explosions, and the timescale from the SN explosion to the peak can be very similar among normal SNe Ia.…”

Section: Implications From the Rise Time Of Normal Sne Iamentioning

confidence: 99%

The HSC-SSP Transient Survey: Implications from Early Photometry and Rise Time of Normal Type Ia Supernovae

Jiang

Yasuda

Maeda

et al. 2020

ApJ

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With a booming number of Type Ia supernovae (SNe Ia) discovered within a few days of their explosions, a fraction of SNe Ia that show luminosity excess in the early phase (early-excess SNe Ia) have been confirmed. In this article, we report early-phase observations of seven photometrically normal SNe Ia (six early detections and one deep non-detection limit) at the COSMOS field through a half-year transient survey as a part of the Hyper Suprime-Cam Subaru Strategic Program (HSC SSP). In particular, a blue light-curve excess was discovered for HSC17bmhk, a normal SN Ia with rise time longer than 18.8 days, during the first four days after the discovery. The blue early excess in optical wavelength can be explained not only by interactions with a non-degenerate companion or surrounding dense circumstellar matter but also radiation powered by radioactive decays of 56 Ni at the surface of the SN ejecta. Given the growing evidence of the early-excess discoveries in normal SNe Ia that have longer rise times than the average and a similarity in the nature of the blue excess to a luminous SN Ia subclass, we infer that early excess discovered in HSC17bmhk and other normal SNe Ia are most likely attributed to radioactive 56 Ni decay at the surface of the SN ejecta. In order to successfully identify normal SNe Ia with early excess similar to that of HSC17bmhk, early UV photometries or high-cadence blue-band surveys are necessary.

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ZTF Early Observations of Type Ia Supernovae. I. Properties of the 2018 Sample

Cited by 99 publications

References 104 publications

SN2019dge: A Helium-rich Ultra-stripped Envelope Supernova

SN2019dge: A Helium-rich Ultra-stripped Envelope Supernova

SN 2020bvc: A Broad-line Type Ic Supernova with a Double-peaked Optical Light Curve and a Luminous X-Ray and Radio Counterpart

The HSC-SSP Transient Survey: Implications from Early Photometry and Rise Time of Normal Type Ia Supernovae

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