The Berkeley sample of Type II supernovae: BVRI light curves and spectroscopy of 55 SNe II

Jaeger, Thomas de; Zheng, W.; Stahl, Benjamin E.; Filippenko, A. V.; Brink, Thomas G.; Bigley, A.; Blanchard, Kyle; Blanchard, P. K.; Bradley, J. Chester; Cargill, Samantha; Casper, Chadwick; Cenko, S. Bradley; Channa, Sanyum; Choi, Byung Yun; Clubb, K. I.; Cobb, B. E.; Cohen, Daniel P.; Kouchkovsky, Maxime de; Ellison, Michael; Falcon, Edward; Fox, O.; Fuller, Kiera; Ganeshalingam, M.; Gould, Carolina; Graham, M. L.; Halevi, Goni; Hayakawa, Kevin T.; Hestenes, Julia; Hyland, Michael; Jeffers, Benjamin T.; Joubert, N.; Kandrashoff, M. T.; Kelly, Patrick L.; Kim, H.; Kim, M.; Kumar, Sahana; Leonard, Erin; Li, G. Z.; Lowe, T.; Lu, Philip; Mason, M.; McAllister, K. J.; Mauerhan, Jon C.; Modjaz, M.; Molloy, Jeffrey; Perley, D.; Pina, Kenia; Poznanski, D.; Ross, Timothy W.; Shivvers, I.; Silverman, J. M.; Soler, Costas; Stegman, Samantha; Taylor, Stephen R.; Tang, Kevin; Wilkins, Andrew; Wang, Xiaofeng; Wang, Xiang-Gao; Yuk, H.; Yunus, Sameen; Zhang, Keto D.

doi:10.1093/mnras/stz2714

Cited by 53 publications

(18 citation statements)

References 126 publications

(216 reference statements)

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“…In particular, SNe II show a reasonably tight (Pearson coefficient r=0.32) correlation between magnitude and luminosity: longer events are dimmer (b=1.14±0.21). This is in agreement with other studies based on much smaller samples (Anderson et al 2014;Sanders et al 2015;Galbany et al 2016a;Rubin & Gal-Yam 2016;Valenti et al 2016;de Jaeger et al 2019).…”

Section: Sne and Luminosity-duration Correlationssupporting

confidence: 94%

The Zwicky Transient Facility Bright Transient Survey. II. A Public Statistical Sample for Exploring Supernova Demographics*

Perley

Fremling

Sollerman

et al. 2020

ApJ

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189

169

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We present a public catalog of transients from the Zwicky Transient Facility (ZTF) Bright Transient Survey, a magnitude-limited (m<19 mag in either the g or r filter) survey for extragalactic transients in the ZTF public stream. We introduce cuts on survey coverage, sky visibility around peak light, and other properties unconnected to the nature of the transient, and show that the resulting statistical sample is spectroscopically 97% complete at <18 mag, 93% complete at <18.5 mag, and 75% complete at <19 mag. We summarize the fundamental properties of this population, identifying distinct duration-luminosity correlations in a variety of supernova (SN) classes and associating the majority of fast optical transients with well-established spectroscopic SN types (primarily SN Ibn and II/IIb). We measure the Type Ia SN and core-collapse (CC) SN rates and luminosity functions, which show good consistency with recent work. About 7% of CCSNe explode in very low-luminosity galaxies (M i >−16 mag), 10% in red-sequence galaxies, and 1% in massive ellipticals. We find no significant difference in the luminosity or color distributions between the host galaxies of SNe Type II and SNe Type Ib/c, suggesting that line-driven wind stripping does not play a major role in the loss of the hydrogen envelope from their progenitors. Future large-scale classification efforts with ZTF and other wide-area surveys will provide highquality measurements of the rates, properties, and environments of all known types of optical transients and limits on the existence of theoretically predicted but as yet unobserved explosions.

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Section: Sne and Luminosity-duration Correlationssupporting

confidence: 94%

The Zwicky Transient Facility Bright Transient Survey. II. A Public Statistical Sample for Exploring Supernova Demographics*

Perley

Fremling

Sollerman

et al. 2020

ApJ

Self Cite

189

169

View full text Add to dashboard Cite

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“…Using only SNe Ia but not combined with measurements of the cosmic microwave background radiation 2. SNe II refer to the two subgroups, SNe IIP and SNe IIL (seeAnderson et al 2014;Sanders et al 2015;Valenti et al 2016;Galbany et al 2016;de Jaeger et al 2019). SNe IIb, SNe IIn, and SN 1987A-like are excluded.…”

mentioning

confidence: 99%

Studying Type II supernovae as cosmological standard candles using the Dark Energy Survey

Jaeger¹,

Galbany

González–Gaitán

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Despite vast improvements in the measurement of the cosmological parameters, the nature of dark energy and an accurate value of the Hubble constant (H0) in the Hubble–Lemaître law remain unknown. To break the current impasse, it is necessary to develop as many independent techniques as possible, such as the use of Type II supernovae (SNe II). The goal of this paper is to demonstrate the utility of SNe II for deriving accurate extragalactic distances, which will be an asset for the next generation of telescopes where more-distant SNe II will be discovered. More specifically, we present a sample from the Dark Energy Survey Supernova Program (DES-SN) consisting of 15 SNe II with photometric and spectroscopic information spanning a redshift range up to 0.35. Combining our DES SNe with publicly available samples, and using the standard candle method (SCM), we construct the largest available Hubble diagram with SNe II in the Hubble flow (70 SNe II) and find an observed dispersion of 0.27 mag. We demonstrate that adding a colour term to the SN II standardization does not reduce the scatter in the Hubble diagram. Although SNe II are viable as distance indicators, this work points out important issues for improving their utility as independent extragalactic beacons: find new correlations, define a more standard subclass of SNe II, construct new SN II templates, and dedicate more observing time to high-redshift SNe II. Finally, for the first time, we perform simulations to estimate the redshift-dependent distance-modulus bias due to selection effects.

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“…The colors of SNe II in the plateau (e.g de Jaeger et al 2019). are similar to those of SESNe around the peak (e.g Drout et al 2011),.…”

mentioning

confidence: 67%

Are stripped envelope supernovae really deficient in $^{56}$Ni?

Ouchi,

Maeda,

Anderson

et al. 2021

Preprint

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Recent works have indicated that the 56 Ni masses estimated for Stripped Envelope SNe (SESNe) are systematically higher than those estimated for SNe II. Although this may suggest a distinct progenitor structure between these types of SNe, the possibility remains that this may be caused by observational bias. One important possible bias is that SESNe with low 56 Ni mass are dim, and therefore they are more likely to escape detection. By investigating the distributions of the 56 Ni mass and distance for the samples collected from the literature, we find that the current literature SESN sample indeed suffers from a significant observational bias, i.e., objects with low 56 Ni mass -if they exist -will be missed, especially at larger distances. Note, however, that those distant objects in our sample are mostly SNe Ic-BL. We also conducted mock observations assuming that the 56 Ni mass distribution for SESNe is intrinsically the same with that for SNe II. We find that the 56 Ni mass distribution of the detected SESNe samples moves toward higher mass than the assumed intrinsic distribution, because of the difficulty in detecting the low-56 Ni mass SESNe. These results could explain the general trend of the higher 56 Ni mass distribution (than SNe II) of SESNe found thus far in the literature. However, further finding clear examples of low-56 Ni mass SESNe (≤ 0.01M ) is required to add weight to this hypothesis. Also, the objects with high 56 Ni mass ( 0.2M ) are not explained by our model, which may require an additional explanation.

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The Berkeley sample of Type II supernovae: BVRI light curves and spectroscopy of 55 SNe II

Cited by 53 publications

References 126 publications

The Zwicky Transient Facility Bright Transient Survey. II. A Public Statistical Sample for Exploring Supernova Demographics*

The Zwicky Transient Facility Bright Transient Survey. II. A Public Statistical Sample for Exploring Supernova Demographics*

Studying Type II supernovae as cosmological standard candles using the Dark Energy Survey

Are stripped envelope supernovae really deficient in $^{56}$Ni?

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