The Zwicky Transient Facility Census of the Local Universe. I. Systematic Search for Calcium-rich Gap Transients Reveals Three Related Spectroscopic Subclasses

De, Kishalay; Kasliwal, Mansi M.; Tzanidakis, Anastasios; Fremling, C.; Adams, S. M.; Andreoni, Igor; Bagdasaryan, Ashot; Bellm, Eric C.; Bildsten, Lars; Cannella, Christopher; Cook, D.; Delacroix, Alexandre; Drake, A. J.; Duev, Dmitry A.; Dugas, A.; Frederick, Sara; Gal‐Yam, A.; Goldstein, Daniel A.; Golkhou, V. Z.; Graham, M. J.; Hale, David; Hankins, Matthew J.; Hélou, G.; Ho, Anna Y. Q.; Irani, I.; Jencson, J.; Kaye, Stephen B.; Kulkarni, S. R.; Kupfer, Thomas; Laher, Russ R.; Leadbeater, R.; Lunnan, R.; Masci, Frank J.; Miller, A. A.; Neill, James D.; Ofek, E. O.; Perley, D.; Polin, Abigail; Prince, Thomas A.; Quataert, Eliot; Reiley, Dan; Riddle, Reed; Rusholme, B.; Sharma, Y.; Shupe, D. L.; Sollerman, J.; Tartaglia, L.; Walters, Richard; Yan, Lin; Yao, Yuhan

doi:10.3847/1538-4357/abb45c

Cited by 82 publications

(73 citation statements)

References 174 publications

(368 reference statements)

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“…Figure 8 shows the number of novae recovered in the first 17 months of the PGIR survey simulation as a function of the input Galactic rate. Similar to the rate estimation procedure discussed in De et al (2020i), we estimate the bestfit rate and its confidence interval by creating a distribution of the fraction of simulations that produce the observed number of novae (= 11) as a function of the global rate. We fit a skewed normal function to this distribution to estimate a Galactic rate (with 68% confidence intervals)…”

Section: Monte Carlo Rate Estimatementioning

confidence: 99%

A Population of Heavily Reddened, Optically Missed Novae from Palomar Gattini-IR: Constraints on the Galactic Nova Rate

Kasliwal

Hankins

et al. 2021

ApJ

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The nova rate in the Milky Way remains largely uncertain, despite its vital importance in constraining models of Galactic chemical evolution as well as understanding progenitor channels for Type Ia supernovae. The rate has been previously estimated to be in the range of ≈10-300 yr −1 , either based on extrapolations from a handful of very bright optical novae or the nova rates in nearby galaxies; both methods are subject to debatable assumptions. The total discovery rate of optical novae remains much smaller (≈5-10 yr −1 ) than these estimates, even with the advent of all-sky optical time-domain surveys. Here, we present a systematic sample of 12 spectroscopically confirmed Galactic novae detected in the first 17 months of Palomar Gattini-IR (PGIR), a wide-field near-infrared time-domain survey. Operating in the J band (≈1.2 μm), which is significantly less affected by dust extinction compared to optical bands, the extinction distribution of the PGIR sample is highly skewed to a large extinction values (>50% of events obscured by A V  5 mag). Using recent estimates for the distribution of Galactic mass and dust, we show that the extinction distribution of the PGIR sample is commensurate with dust models. The PGIR extinction distribution is inconsistent with that reported in previous optical searches (null-hypothesis probability <0.01%), suggesting that a large population of highly obscured novae have been systematically missed in previous optical searches. We perform the first quantitative simulation of a 3π time-domain survey to estimate the Galactic nova rate using PGIR, and derive a rate of » -+ 43.7 8.719.5 yr −1 . Our results suggest that all-sky near-infrared timedomain surveys are well poised to uncover the Galactic nova population.

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Section: Monte Carlo Rate Estimatementioning

confidence: 99%

A Population of Heavily Reddened, Optically Missed Novae from Palomar Gattini-IR: Constraints on the Galactic Nova Rate

Kasliwal

Hankins

et al. 2021

ApJ

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“…Our current sample of Ca-rich SNe offsets is based on the sample from our original characterization study (Perets et al 2010) based on SNe from the LOSS and CCCP surveys, and the additional Ca-rich SNe discovered by the PTF/iPTF (Kasliwal et al 2012;Lunnan et al 2017;De et al 2018), PESSTO (Valenti et al 2014) and ZTF (De et al 2020;Jacobson-Galán et al 2020 surveys. The SNe offsets are taken from these studies, and summarized in Table 1; the cumulative The cumulative offset distributions of sGRBs and Ca-rich supernovae in early-and late-type galaxies.…”

Section: Ca-rich Supernovae Samplementioning

confidence: 99%

“…The majority of Ca-rich SNe were found in old stellar populations in early-type galaxies (e.g. Perets et al 2010;De et al 2020) it was therefore expected that the locations and offsets of such SNe in their host galaxies would follow the old stellar populations in these galaxies. However, many of the SNe both in our original (Perets et al 2010) sample and additional Ca-rich SNe identified later on (Kasliwal et al 2012;De et al 2020) were found at large offsets from their host galaxies (see Table 1 and Fig.…”

Section: The Progenitors Of Ca-rich Supernovaementioning

confidence: 99%

“…This is consistent with the suggested NS mergers and thermonuclear WD explosions which can indeed have very long delay-time since the formation of their progenitor stars. However, in many cases, not only were these transients far from any star-forming regions, but they also appeared to be located very far from their host galaxies (Perets et al 2010;Kasliwal et al 2012;Fong & Berger 2013;Fong et al 2017;Lunnan et al 2017;De et al 2020). It was therefore suggested by several studies that the remote locations of such transients could be explained either by large velocity kicks given to their progenitors ( (Lyman et al 2014;Foley 2015;Lyman et al 2016) for Ca-rich SNe; (Fong & Berger 2013) for sGRBs), or that the progenitors form in dense globular clusters, since many of those reside in the haloes (Yuan et al 2013;Sell et al 2015;Shen, Quataert & Pakmor 2019).…”

Section: Introductionmentioning

confidence: 99%

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No velocity-kicks are required to explain large-distance offsets of Ca-rich supernovae and short-GRBs

Perets

Beniamini

2021

Monthly Notices of the Royal Astronomical Society

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Environments of supernovae (SNe) and gamma-ray bursts (GRBs) link their progenitors to the underlying stellar population, providing critical clues for their origins. However, various transients including Ca-rich SNe and short-GRBs, appear to be located at remote locations, far from the stellar population of their host galaxy, challenging our understanding of their origin and/or physical evolution. These findings instigated models suggesting that either large velocity-kicks were imparted to the transient progenitors, allowing them to propagate to large distances and attain their remote locations; or that they formed in dense globular-clusters residing in the haloes. Here we show that instead, large spatial-offsets of such transients are naturally explained by observations of highly extended stellar populations in (mostly early-type) galaxy haloes, typically missed since they can only be identified through ultra-deep/stacked images. Consequently, no large velocity kicks, nor halo globular-cluster environments are required in order to explain the origin of these transients. These findings support thermonuclear explosions on white-dwarfs, for the origins of Ca-rich SNe progenitors, and the existence of small (or zero) kick-velocities given to short-GRB progenitors. Furthermore, since stacked/ultra-deep imaging show that early-type galaxies are more extended than late-type galaxies, studies of transients’ offset-distribution (e.g. type Ia SNe or FRBs) should account for host galaxy-type. Since early-type galaxies contain older stellar populations, transient arising from older stellar populations would have larger fractions of early-type hosts, and consequently larger fractions of large-offset transients. In agreement with out results for short-GRBs and Ca-rich SNe showing different offset distributions in early versus late-type galaxies.

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“…Figure 2 shows the light curve produced from the PGIR forced photometry pipeline. Point-spread function (PSF) fit photometry is performed, with noise uncertainty at the location of the transient estimated, as described in De et al (2020b), from difference images produced using the ZOGY algorithm (Zackay et al 2016).…”

Section: Gattini 12 μM (J-band) Light Curvementioning

confidence: 99%

Outbursting Young Stellar Object PGIR 20dci in the Perseus Arm

Hillenbrand

Hankins

et al. 2021

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We report the discovery of a likely outbursting Class I young stellar object, associated with the star-forming region NGC 281-W (distance ∼2.8 kpc). The source is currently seen only at infrared wavelengths, appearing in both the Palomar Gattini InfraRed (1.2 μm) and the Near-Earth Object Wide-field Infrared Survey Explorer (3.4 and 4.6 μm) photometric time-domain surveys. Recent near-infrared imaging reveals a new, extended scattered light nebula. Recent near-infrared spectroscopy confirms the similarity of PGIR 20dci to FU Ori-type sources, based on strong molecular absorption in CO, H 2 O, and OH; weak absorption in several atomic lines; and a warm wind/ outflow as indicated by a P Cygni profile in the He I λ10830 line. This is a rare case of an FU Ori star with a wellmeasured long-term photometric rise before a sharper outburst, and the second instance of an FU Ori star with a documented two-step brightening in the mid-infrared.

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The Zwicky Transient Facility Census of the Local Universe. I. Systematic Search for Calcium-rich Gap Transients Reveals Three Related Spectroscopic Subclasses

Cited by 82 publications

References 174 publications

A Population of Heavily Reddened, Optically Missed Novae from Palomar Gattini-IR: Constraints on the Galactic Nova Rate

A Population of Heavily Reddened, Optically Missed Novae from Palomar Gattini-IR: Constraints on the Galactic Nova Rate

No velocity-kicks are required to explain large-distance offsets of Ca-rich supernovae and short-GRBs

Outbursting Young Stellar Object PGIR 20dci in the Perseus Arm

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