High-resolution spectroscopy of SN 2017hcc and its blueshifted line profiles from post-shock dust formation

Smith, Nathan; Andrews, Jennifer E.

doi:10.1093/mnras/staa3047

Cited by 13 publications

(28 citation statements)

References 118 publications

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“…Based on this picture, the decline rates of these SNe may hint that the level of CSM interaction continuously decreases in the last years (except in the case of SN 2010mc, which seems to be in a very long "plateau" phase even at ∼3000 days). SN 2017hcc stands out among our LASTCHANCE sample because of its unusually high degree of polarization (Mauerhan et al 2017;Kumar et al 2019) and the post-shock dust formation assumed from the analysis of its strongly blueshifted line profiles (Smith & Andrews 2020). The SN was observed at three epochs (392, 565, and 767 days) by Spitzer.…”

Section: Type Iin Snementioning

confidence: 99%

Spitzer’s Last Look at Extragalactic Explosions: Long-term Evolution of Interacting Supernovae

Szalai

Fox

Arendt³

et al. 2021

ApJ

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Here we present new, yet final, mid-infrared (mid-IR) data for supernovae (SNe) based on measurements with the Spitzer Space Telescope. Comparing our recent 3.6 and 4.5 μm photometry with previously published mid-IR and further multiwavelength data sets, we were able to draw some conclusions about the origin and heating mechanism of the dust in these SNe or in their environments, as well as about possible connection with circumstellar matter (CSM) originating from pre-explosion mass-loss events in the progenitor stars. We also present new results regarding both certain SN classes and single objects. We highlight the mid-IR homogeneity of SNe Ia-CSM, which may be a hint of their common progenitor type and of their basically uniform circumstellar environments. Regarding single objects, it is worth highlighting the late-time interacting Type Ib SNe 2003gk and 2004dk, for which we present the first-ever mid-IR data, which seem to be consistent with clues of ongoing CSM interaction detected in other wavelength ranges. Our current study suggests that long-term mid-IR follow-up observations play a key role in a better understanding of both pre-and post-explosion processes in SNe and their environments. While Spitzer is not available anymore, the expected unique data from the James Webb Space Telescope, as well as long-term near-IR follow-up observations of dusty SNe, can bring us closer to the hidden details of this topic.Unified Astronomy Thesaurus concepts: Supernovae (1668); Infrared astronomy (786); Infrared telescopes (794); Circumstellar matter (241); Circumstellar dust (236)

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Section: Type Iin Snementioning

confidence: 99%

Spitzer’s Last Look at Extragalactic Explosions: Long-term Evolution of Interacting Supernovae

Szalai

Fox

Arendt³

et al. 2021

ApJ

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“…Studies of dust across a range of environments, from the SMC (Welty et al 2006(Welty et al , 2012 to the ISM of QSO host galaxies (Baron et al 2016), have likewise indicated that E(B −V ) values of 0.05 mag are associated with higher W r (Na I) than implied by Poznanski et al (2012). As the Poznanski et al (2012) relation is commonly invoked to estimate the reddening of both type I and II supernovae in combination with measurements of W r (Na I) in spectroscopy of these objects (e.g., Smith & Andrews 2020;Bruch et al 2021;Dastidar et al 2021), it is important to appreciate potential biases that may arise from this calibration (e.g., Phillips et al 2013). Moreover, given the wide range in stellar masses of our GOTOQ host galaxies, we suggest that our sample may better represent the varied dust and ISM properties of supernova host galaxies than those focused purely on the Milky Way, SMC, or QSO host systems.…”

Section: Relation Between W R and Dust Reddeningmentioning

confidence: 95%

On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies

Rubin

Juarez

Cooksey

et al. 2022

ApJ

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We use medium-resolution Keck/Echellette Spectrograph and Imager spectroscopy of bright quasars to study cool gas traced by Ca ii λλ3934, 3969 and Na i λλ5891, 5897 absorption in the interstellar/circumgalactic media of 21 foreground star-forming galaxies at redshifts 0.03 < z < 0.20 with stellar masses 7.4 ≤ log M */M ⊙ ≤ 10.6. The quasar–galaxy pairs were drawn from a unique sample of Sloan Digital Sky Survey quasar spectra with intervening nebular emission, and thus have exceptionally close impact parameters (R ⊥ < 13 kpc). The strength of this line emission implies that the galaxies’ star formation rates (SFRs) span a broad range, with several lying well above the star-forming sequence. We use Voigt profile modeling to derive column densities and component velocities for each absorber, finding that column densities N(Ca ii) > 1012.5 cm−2 (N(Na i) > 1012.0 cm−2) occur with an incidence f C(Ca ii) = 0.63+0.10 −0.11 (f C(Na i) = 0.57+0.10 −0.11). We find no evidence for a dependence of f C or the rest-frame equivalent widths W r (Ca ii K) or W r (Na i 5891) on R ⊥ or M *. Instead, W r (Ca ii K) is correlated with local SFR at >3σ significance, suggesting that Ca ii traces star formation-driven outflows. While most of the absorbers have velocities within ±50 km s−1 of the host redshift, their velocity widths (characterized by Δv 90) are universally 30–177 km s−1 larger than that implied by tilted-ring modeling of the velocities of interstellar material. These kinematics must trace galactic fountain flows and demonstrate that they persist at R ⊥ > 5 kpc. Finally, we assess the relationship between dust reddening and W r (Ca ii K) (W r (Na i 5891)), finding that 33% (24%) of the absorbers are inconsistent with the best-fit Milky Way E(B−V)-W r relations at >3σ significance.

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“…They also estimated a mass-loss rate of 𝑀 = 0.12 𝑀 yr −1 (for a wind speed of 20 km s −1 ), which is comparable to the mass-loss rate for an LBV in eruption. However, based on echelle spectra, Smith & Andrews (2020) suggested the CSM wind to be flowing axi-symmetrically with wind speeds of 𝑣 𝑤 = 40 − 50 km s −1 indicating bipolar geometry of the CSM created by losing 10 𝑀 of stellar mass to eruptive mass ejections. Smith & Andrews (2020) modeled the optical and near IR emission of SN 2017hcc and found indications that the SN ejecta were hidden behind the photosphere until day 75.…”

Section: Introductionmentioning

confidence: 99%

“…However, based on echelle spectra, Smith & Andrews (2020) suggested the CSM wind to be flowing axi-symmetrically with wind speeds of 𝑣 𝑤 = 40 − 50 km s −1 indicating bipolar geometry of the CSM created by losing 10 𝑀 of stellar mass to eruptive mass ejections. Smith & Andrews (2020) modeled the optical and near IR emission of SN 2017hcc and found indications that the SN ejecta were hidden behind the photosphere until day 75. They found that the early time symmetric profiles changed to asymmetric blueshifted profiles at late times.…”

Section: Introductionmentioning

confidence: 99%

The luminous type IIn supernova SN 2017hcc: Infrared bright, X-ray, and radio faint

Chandra

Chevalier

James

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present multiwavelength observations of supernova (SN) 2017hcc with the Chandra X-ray telescope and the X-ray telescope onboard Swift (Swift-XRT) in X-ray bands, with the Spitzer and the TripleSpec spectrometer in near-infrared (IR) and mid-IR bands and with the Karl G. Jansky Very Large Array (VLA) for radio bands. The X-ray observations cover a period of 29 to 1310 days, with the first X-ray detection on day 727 with the Chandra. The SN was subsequently detected in the VLA radio bands from day 1000 onwards. While the radio data are sparse, synchrotron-self absorption is clearly ruled out as the radio absorption mechanism. The near- and the mid-IR observations showed that late time IR emission dominates the spectral energy distribution. The early properties of SN 2017hcc are consistent with shock breakout into a dense mass-loss region, with $\dot{M} \sim 0.1$M⊙ yr−1 for a decade. At few 100 days, the mass-loss rate declined to ∼0.02 M⊙ yr−1, as determined from the dominant IR luminosity. In addition, radio data also allowed us to calculate a mass-loss rate at around day 1000, which is two orders of magnitude smaller than the mass-loss rate estimates around the bolometric peak. These values indicate that the SN progenitor underwent an enhanced mass-loss event a decade before the explosion. The high ratio of IR to X-ray luminosity is not expected in simple models and is possible evidence for an asymmetric circumstellar region.

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High-resolution spectroscopy of SN 2017hcc and its blueshifted line profiles from post-shock dust formation

Cited by 13 publications

References 118 publications

Spitzer’s Last Look at Extragalactic Explosions: Long-term Evolution of Interacting Supernovae

Spitzer’s Last Look at Extragalactic Explosions: Long-term Evolution of Interacting Supernovae

On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies

The luminous type IIn supernova SN 2017hcc: Infrared bright, X-ray, and radio faint

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