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Journal articles on the topic 'Supernova spectroscopy'

Author: Grafiati

Published: 10 December 2022

Last updated: 19 July 2025

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1

Chevalier, R. A. "The Early Evolution of Supernova Remnants." International Astronomical Union Colloquium 101 (1988): 31–42. http://dx.doi.org/10.1017/s0252921100102076.

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AbstractThe density distribution of the supernova ejecta and that of the surrounding medium are the most important parameters for the early evolution of supernova remnants. The distribution of the ejecta depends on the detailed hydrodynamics of the explosion, but the outer parts of a supernova can probably be represented by a steep power law density distribution with radius. Self-similar solutions are especially useful for modeling the interaction of a supernova with its surrounding. The supernova first interacts with mass loss from the progenitor star. Evidence for circumstellar interaction is present in a number of extragalactic supernovae, including SN1987a. The explosions of massive stars probably interact with circumstellar gas for a considerable time while Type Ia supernovae interact more directly with the interstellar medium. X-ray spectroscopy is a good diagnostic for the physical conditions in young supernova remnants and for the composition of the supernova gas.

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2

Arcavi, Iair. "Type II SN Light Curves from the Caltech Core Collapse Project." Proceedings of the International Astronomical Union 7, S285 (2011): 431–53. http://dx.doi.org/10.1017/s1743921312001329.

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We presented our analysis of a sample of type II supernova (SN) light curves measured by the Caltech Core Collapse Project (CCCP). CCCP is a large observational program which made use of the robotic 60-in and the Hale 200-in telescopes to obtain optical photometry, spectroscopy and IR photometry of 49 nearby core-collapse supernovae (SNe). It provides a fair sample of core-collapse events, with well-defined selection criteria, and uniform, high-quality optical/IR observations. Our goal is to characterize the little-studied properties of core-collapse supernovae as a population. Preliminary data indicate a diverse set of sub-populations including “standard” type IIP supernovæ, declining supernovæ (at different rates) and slowly rising peculiar supernovæ. Work is in progress to map and quantify that diversity better. It is hoped that a single tunable formula will be able to describe most light-curve shapes, thereby helping us attain a better understanding of the physical mechanisms underlying these results.

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3

Anderson, Joseph P., Stacey M. Habergham, Phil A. James, and M. Hamuy. "The Local Environments of Core-Collapse SNe within Host Galaxies." Proceedings of the International Astronomical Union 7, S279 (2011): 183–86. http://dx.doi.org/10.1017/s1743921312012896.

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AbstractWe present constraints on core-collapse supernova progenitors through observations of their environments within host galaxies. This is achieved through 2 routes. Firstly, we investigate the spatial correlation of supernovae with host galaxy star formation using pixel statistics. We find that the main supernova types form a sequence of increasing association to star formation. The most logical interpretation is that this implies an increasing progenitor mass sequence going from the supernova type Ia arising from the lowest mass, through the type II, type Ib, and the supernova type Ic arising from the highest mass progenitors. We find the surprising result that the supernova type IIn show a lower association to star formation than type IIPs, implying lower mass progenitors. Secondly, we use host HII region spectroscopy to investigate differences in environment metallicity between different core-collapse types. We find that supernovae of types Ibc arise in slightly higher metallicity environments than type II events. However, this difference is not significant, implying that progenitor metallicity does not play a dominant role in deciding supernova type.

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4

Kuncarayakti, Hanindyo. "The explosion sites of nearby supernovae seen with integral field spectroscopy." Proceedings of the International Astronomical Union 11, A29B (2015): 276–77. http://dx.doi.org/10.1017/s1743921316005330.

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AbstractIntegral field spectroscopy of nearby supernova sites within ~30 Mpc have been obtained using multiple IFU spectrographs in Hawaii and Chile. This technique enables both spatial and spectral information of the explosion sites to be acquired simultaneously, thus providing the identification of the parent stellar population of the supernova progenitor and the estimates for its physical parameters including age and metallicity via the spectrum. While this work has mainly been done in the optical wavelengths using instruments such as VIMOS, GMOS, and MUSE, a near-infrared approach has also been carried out using the AO-assisted SINFONI. By studying the supernova parent stellar population, we aim to characterize the mass and metallicity of the progenitors of different types of supernovae.

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5

Kuncarayakti, Hanindyo, Mamoru Doi, Greg Aldering, et al. "Mass and metallicity constraints on supernova progenitors derived from integral field spectroscopy of the environment." Proceedings of the International Astronomical Union 7, S279 (2011): 343–44. http://dx.doi.org/10.1017/s1743921312013269.

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AbstractWe have obtained optical integral field spectroscopy of the explosion sites of more than 25 nearby type-IIP/IIL/Ib/Ic supernovae using UH88/SNIFS, and additionally Gemini/GMOS IFU. This technique enables us to obtain both spatial and spectral information of the immediate environment of the supernovae. Using strong line method we measured the metallicity of the star cluster present at the explosion site, presumably the coeval parent stellar population of the supernova progenitor, and comparison with simple stellar population models gives age estimate of the cluster. With this method we were able to put constraints on the metallicity and age of the progenitor star. The age, i.e. lifetime, of the progenitor corresponds to the initial mass of the star. By far this is the most direct measurement of supernova progenitor metallicity and, if the cluster-progenitor association is confirmed, provides reliable determination of the initial mass of supernova progenitor stars.

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6

Chevalier, R. A. "High-energy Emission from Supernovae and Remnants." Symposium - International Astronomical Union 195 (2000): 135–42. http://dx.doi.org/10.1017/s0074180900162874.

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An early burst of energetic radiation is expected from a supernova at the time of shock breakout. This emission has not been directly observed but has been inferred from the photoionization around SN 1987A. X-ray emission has been detected from core-collapse supernovae in the days to years after the explosion as they interact with their circumstellar winds. Young Galactic supernova remnants provide the possibility of determining the composition structure of the ejecta through X-ray spectroscopy. An exciting finding for older remnants is that a number of remnants that appear to be interacting with molecular gas may be sources of high-energy γ-ray emission. The clumpy structure of molecular clouds has implications for the structure expected in high-energy emission. Finally, the field of γ-ray-line spectroscopy is beginning to yield results relevant to the explosive nucleosynthesis of radionuclides in supernovae.

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7

Ellis, Richard, and Mark Sullivan. "Verifying the Use of Supernovae as Probes of the Cosmic Expansion." Symposium - International Astronomical Union 201 (2005): 231–40. http://dx.doi.org/10.1017/s007418090021629x.

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We present preliminary results of a follow-up survey which aims to characterise in detail those galaxies which hosted Type Ia supernovae found by the Supernova Cosmology Project. Our survey has two components: Hubble Space Telescope imaging with STIS and Keck spectroscopy with ESI, the goal being to classify each host galaxy into one of three broad morphological/spectral classes and hence to investigate the dependence of supernovae properties on host galaxy type over a large range in redshift. Of particular interest is the supernova Hubble diagram characterised by host galaxy class which suggests that most of the scatter arises from those occurring in late-type irregulars. Supernovae hosted by (presumed dust-free) E/SO galaxies closely follow the adopted SCP cosmological model. Although larger datasets are required, we cannot yet find any significant difference in the light curves of distant supernovae hosted in different galaxy types.

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8

Folatelli, Gastón, Nidia Morrell, Mark M. Phillips, et al. "SPECTROSCOPY OF TYPE Ia SUPERNOVAE BY THE CARNEGIE SUPERNOVA PROJECT." Astrophysical Journal 773, no. 1 (2013): 53. http://dx.doi.org/10.1088/0004-637x/773/1/53.

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9

P. Kirshner, Robert. "Supernovae and the Cosmic Distance Scale." International Astronomical Union Colloquium 145 (1996): 19–28. http://dx.doi.org/10.1017/s0252921100007879.

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Knowledge of the size and age of the Universe depends on understanding supernovae. The direct geometric measurement of the circumstellar ring of SN 1987A using IUE spectra and HST images provides an independent test of the Cepheid distance scale to the Large Magellanic Cloud. Understanding the details of the mass distribution in the circumstellar matter is important to improving the precision of this distance. Type la supernovae have a narrow distribution in absolute magnitude, and new Cepheid distances to IC 4182 (the site of SN 1937C) and to NGC 5253 (the site of SN 1972E) obtained with HST by Sandage and his collaborators allow that absolute magnitude to be calibrated. Comparison with more distant SNIa gives H0 = 56 ± 8 km s-1 Mpc-1. Recent work in supernova spectroscopy and photometry shows that the apparent homogeneity of SNIa is not quite what it seems, and a deeper understanding of these variations is needed to use the SNIa to best advantage. The Expanding Photosphere Method (EPM) allows direct measurement to each Type II supernova that has adequate photometry and spectroscopy. There are now 18 such objects. The sample of EPM distances from 4.5 Mpc to 180 Mpc indicates H0 = 73±6 (statistical) ±7 (systematic) km s-1 Mpc-1. Better understanding of supernova atmospheres can reduce the systematic error in this approach, which is completely independent of all other astronomical distances.

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10

Howell, D. A., M. Sullivan, K. Perrett, et al. "Gemini Spectroscopy of Supernovae from the Supernova Legacy Survey: Improving High‐Redshift Supernova Selection and Classification." Astrophysical Journal 634, no. 2 (2005): 1190–201. http://dx.doi.org/10.1086/497119.

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11

Stritzinger, M. D., J. P. Anderson, C. Contreras, et al. "The Carnegie Supernova Project I." Astronomy & Astrophysics 609 (January 2018): A134. http://dx.doi.org/10.1051/0004-6361/201730842.

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The first phase of the Carnegie Supernova Project (CSP-I) was a dedicated supernova follow-up program based at the Las Campanas Observatory that collected science data of young, low-redshift supernovae between 2004 and 2009. Presented in this paper is the CSP-I photometric data release of low-redshift stripped-envelope core-collapse supernovae. The data consist of optical (uBgVri) photometry of 34 objects, with a subset of 26 having near-infrared (YJH) photometry. Twenty objects have optical pre-maximum coverage with a subset of 12 beginning at least five days prior to the epoch of B-band maximum brightness. In the near-infrared, 17 objects have pre-maximum observations with a subset of 14 beginning at least five days prior to the epoch of J-band maximum brightness. Analysis of this photometric data release is presented in companion papers focusing on techniques to estimate host-galaxy extinction and the light-curve and progenitor star properties of the sample. The analysis of an accompanying visual-wavelength spectroscopy sample of ~150 spectra will be the subject of a future paper.

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12

Shahbandeh, M., E. Y. Hsiao, C. Ashall, et al. "Carnegie Supernova Project-II: Near-infrared Spectroscopy of Stripped-envelope Core-collapse Supernovae*." Astrophysical Journal 925, no. 2 (2022): 175. http://dx.doi.org/10.3847/1538-4357/ac4030.

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Abstract We present 75 near-infrared (NIR; 0.8−2.5 μm) spectra of 34 stripped-envelope core-collapse supernovae (SESNe) obtained by the Carnegie Supernova Project-II (CSP-II), encompassing optical spectroscopic Types IIb, Ib, Ic, and Ic-BL. The spectra range in phase from pre-maximum to 80 days past maximum. This unique data set constitutes the largest NIR spectroscopic sample of SESNe to date. NIR spectroscopy provides observables with additional information that is not available in the optical. Specifically, the NIR contains the strong lines of He i and allows a more detailed look at whether Type Ic supernovae are completely stripped of their outer He layer. The NIR spectra of SESNe have broad similarities, but closer examination through statistical means reveals a strong dichotomy between NIR “He-rich” and “He-poor” SNe. These NIR subgroups correspond almost perfectly to the optical IIb/Ib and Ic/Ic-BL types, respectively. The largest difference between the two groups is observed in the 2 μm region, near the He i λ2.0581 μm line. The division between the two groups is not an arbitrary one along a continuous sequence. Early spectra of He-rich SESNe show much stronger He i λ2.0581 μm absorption compared to the He-poor group, but with a wide range of profile shapes. The same line also provides evidence for trace amounts of He in half of our SNe in the He-poor group.

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13

De, K., M. M. Kasliwal, E. O. Ofek, et al. "A hot and fast ultra-stripped supernova that likely formed a compact neutron star binary." Science 362, no. 6411 (2018): 201–6. http://dx.doi.org/10.1126/science.aas8693.

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Compact neutron star binary systems are produced from binary massive stars through stellar evolution involving up to two supernova explosions. The final stages in the formation of these systems have not been directly observed. We report the discovery of iPTF 14gqr (SN 2014ft), a type Ic supernova with a fast-evolving light curve indicating an extremely low ejecta mass (≈0.2 solar masses) and low kinetic energy (≈2 × 1050ergs). Early photometry and spectroscopy reveal evidence of shock cooling of an extended helium-rich envelope, likely ejected in an intense pre-explosion mass-loss episode of the progenitor. Taken together, we interpret iPTF 14gqr as evidence for ultra-stripped supernovae that form neutron stars in compact binary systems.

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14

Krauss, Lawrence M. "Neutrino spectroscopy of supernova 1987A." Nature 329, no. 6141 (1987): 689–94. http://dx.doi.org/10.1038/329689a0.

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15

Moorwood, A. F. M., E. Oliva, and I. J. Danziger. "Infrared Spectroscopy of Supernova Remnants." International Astronomical Union Colloquium 101 (1988): 391–94. http://dx.doi.org/10.1017/s0252921100102714.

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AbstractSpectra of several galactic and LMC supernova remnants have been obtained at R ~ 1500 in the 1−2.5 µm region with the cooled grating/array spectrometer, IRSPEC, on the ESO 3.6m telescope. The brightest lines observed are from [FeII]. In RCW 103, which exhibits the highest surface brightness, H (Brγ at 2.17µm) and H2 (1−0 S(1) at 2.12µm) lines have also been detected. A good correlation is found between [FeII] (1.64µm) and Hβ implying similar ionization structures and Fe abundances in a wide variety of remnants. The actual [FeII](1.64µm)/Hβ ratio of ~0.2 also implies a high depletion factor (>0.9) for Fe. Electron densities, extinctions and [FeII] luminosities derived from these data are presented and discussed and attention drawn to a potentially interesting discrepancy between H(Brγ) and Hβ fluxes.

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16

Spyromilio, Jason. "Infrared Spectroscopy of SN 1987A." International Astronomical Union Colloquium 145 (1996): 193–99. http://dx.doi.org/10.1017/s025292110000806x.

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Infrared spectra of SN 1987A have been obtained at the Anglo-Australian Telescope since the explosion of this supernova. I present highlights from this program which include the analysis of the molecular emission, the determination of the mass of 57Co in the ejecta and the analysis of the emission due to dust in the ejecta. I also show the spectrum of the supernova in the infrared 5 years after explosion.

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17

Chandra, Vedant, Hsiang-Chih Hwang, Nadia L. Zakamska, et al. "The SN Ia runaway LP 398-9: detection of circumstellar material and surface rotation." Monthly Notices of the Royal Astronomical Society 512, no. 4 (2022): 6122–33. http://dx.doi.org/10.1093/mnras/stac883.

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ABSTRACT A promising progenitor scenario for Type Ia supernovae (SNeIa) is the thermonuclear detonation of a white dwarf in a close binary system with another white dwarf. After the primary star explodes, the surviving donor can be spontaneously released as a hypervelocity runaway. One such runaway donor candidate is LP 398-9, whose orbital trajectory traces back ≈105 yr to a known supernova remnant. Here, we report the discovery of carbon-rich circumstellar material around LP 398-9, revealed by a strong infrared excess and analysed with follow-up spectroscopy. The circumstellar material is most plausibly composed of inflated layers from the star itself, mechanically and radioactively heated by the past companion’s supernova. We also detect a 15.4 h periodic signal in the UV and optical light curves of LP 398-9, which we interpret as surface rotation. The rotation rate is consistent with theoretical predictions from this supernova mechanism, and the brightness variations could originate from surface inhomogeneity deposited by the supernova itself. Our observations strengthen the case for this double-degenerate SNIa progenitor channel, and motivate the search for more runaway SNIa donors.

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Raddi, R., M. A. Hollands, D. Koester, et al. "Partly burnt runaway stellar remnants from peculiar thermonuclear supernovae." Monthly Notices of the Royal Astronomical Society 489, no. 2 (2019): 1489–508. http://dx.doi.org/10.1093/mnras/stz1618.

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Abstract We report the discovery of three stars that, along with the prototype LP 40−365, form a distinct class of chemically peculiar runaway stars that are the survivors of thermonuclear explosions. Spectroscopy of the four confirmed LP 40−365 stars finds ONe-dominated atmospheres enriched with remarkably similar amounts of nuclear ashes of partial O- and Si-burning. Kinematic evidence is consistent with ejection from a binary supernova progenitor; at least two stars have rest-frame velocities indicating they are unbound to the Galaxy. With masses and radii ranging between 0.20 and 0.28 M$\odot$ and between 0.16 and 0.60 R$\odot$, respectively, we speculate these inflated white dwarfs are the partly burnt remnants of either peculiar Type Iax or electron-capture supernovae. Adopting supernova rates from the literature, we estimate that ∼20 LP 40−365 stars brighter than 19 mag should be detectable within 2 kpc from the Sun at the end of the Gaia mission. We suggest that as they cool, these stars will evolve in their spectroscopic appearance, and eventually become peculiar O-rich white dwarfs. Finally, we stress that the discovery of new LP 40−365 stars will be useful to further constrain their evolution, supplying key boundary conditions to the modelling of explosion mechanisms, supernova rates, and nucleosynthetic yields of peculiar thermonuclear explosions.

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19

Morrell, N., M. M. Phillips, G. Folatelli, et al. "Optical Spectroscopy of Type Ia Supernovae by the Carnegie Supernova Projects I and II." Astrophysical Journal 967, no. 1 (2024): 20. http://dx.doi.org/10.3847/1538-4357/ad38af.

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Abstract We present the second and final release of optical spectroscopy of Type Ia supernovae (SNe Ia) obtained during the first and second phases of the Carnegie Supernova Project (CSP-I and CSP-II). The newly released data consist of 148 spectra of 30 SNe Ia observed in the course of CSP-I and 234 spectra of 127 SNe Ia obtained during CSP-II. We also present 216 optical spectra of 46 historical SNe Ia, including 53 spectra of 30 SNe Ia observed by the Calán/Tololo Supernova Survey. We combine these observations with previously published CSP data and publicly available spectra to compile a large sample of measurements of spectroscopic parameters at maximum light, consisting of pseudo-equivalent widths and expansion velocities of selected features for 232 CSP and historical SNe Ia (including more than 1000 spectra). Finally, we review some of the strongest correlations between spectroscopic and photometric properties of SNe Ia. Specifically, we define two samples: one consisting of SNe Ia discovered by targeted searches (most of them CSP-I objects) and the other composed of SNe Ia discovered by untargeted searches, which includes most of the CSP-II objects. The analyzed correlations are similar for both samples. We find a larger incidence of SNe Ia belonging to the cool and broad-line Branch subtypes among the events discovered by targeted searches, shallow-silicon SNe Ia are present with similar frequencies in both samples, while core normal SNe Ia are more frequent in untargeted searches.

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20

Dutta, Anirban, Avinash Singh, G. C. Anupama, D. K. Sahu, and Brajesh Kumar. "SN 2017hpa: a carbon-rich Type Ia supernova." Monthly Notices of the Royal Astronomical Society 503, no. 1 (2021): 896–910. http://dx.doi.org/10.1093/mnras/stab481.

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ABSTRACT We present the optical (UBVRI) and ultraviolet (Swift-Ultraviolet and Optical Telescope) photometry, and optical spectroscopy of Type Ia supernova SN 2017hpa. We study broad-band ultraviolet (UV)+optical light curves and low-resolution spectroscopy spanning from −13.8 to +108 d from the maximum light in B band. The photometric analysis indicates that SN 2017hpa is a normal Type Ia supernova with ΔmB(15) = 0.98 ± 0.16 mag and MB = −19.45 ± 0.15 mag at a distance modulus of μ = 34.08 ± 0.09 mag. The (uvw1 − uvv) colour evolution shows that SN 2017hpa falls in the near-UV (NUV)-blue group. The (B − V) colour at maximum is bluer in comparison to normal Type Ia supernovae. Spectroscopic analysis shows that the Si ii λ6355 Å absorption feature evolves rapidly with a velocity gradient, $\dot{v}=128\pm 7$ km s−1 d−1. The pre-maximum phase spectra show prominent C ii λ6580 Å absorption feature. The C ii 6580 Å line velocity measured from the observed spectra is lower than the velocity of Si ii λ6355 Å, which could be due to a line-of-sight effect. The synthetic spectral fits to the pre-maximum spectra using syn++ indicate the presence of a high-velocity component in the Si ii absorption, in addition to a photospheric component. Fitting the observed spectrum with the spectral synthesis code tardis, the mass of unburned C in the ejecta is estimated to be ∼0.019 M⊙. The peak bolometric luminosity is $L^{\rm {bol}}_{\rm {peak}} = 1.43\times 10^{43}$ erg s−1. The radiation diffusion model fit to the bolometric light curve indicates 0.61 ± 0.02 M⊙ of 56Ni is synthesized in the explosion.

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21

Kochanek, C. S. "The physics of flash (supernova) spectroscopy." Monthly Notices of the Royal Astronomical Society 483, no. 3 (2018): 3762–72. http://dx.doi.org/10.1093/mnras/sty3363.

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22

Reach, William T., and Jeonghee Rho. "Infrared Spectroscopy of Molecular Supernova Remnants." Astrophysical Journal 558, no. 2 (2001): 943. http://dx.doi.org/10.1086/322391.

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23

Petre, R. "X-Ray Spectroscopy of Supernova Remnants." International Astronomical Union Colloquium 145 (1996): 357–68. http://dx.doi.org/10.1017/s0252921100008216.

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X-ray spectroscopy can provide vital information about the progenitors and environments of supernova remnants. Plasma diagnostics and spectral modelling can be used to infer the energy of the remnant, the density and composition of the surrounding medium, and the degree of equilibrium in the shock heated gas. A new generation of X-ray spectrometers, the first of which was the Broad-Band X-Ray Telescope (BBXRT), has improved our ability to make precise measurements of X-ray line fluxes and energies. We summarize the results obtained from the BBXRT mission. These include a definitive measurement of the Fe K line centroid in the Tycho remnant, production of the first narrow-band X-ray maps (of Puppis A) and the first measurement of an electron-ion equipartition timescales in evolved remnants.

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24

Tyson, J. Anthony, and Patricia C. Boeshaar. "Early optical spectroscopy of supernova 1987A." Publications of the Astronomical Society of the Pacific 99 (September 1987): 905. http://dx.doi.org/10.1086/132057.

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Ballet, Jean, and Anne Decourchelle. "X-ray spectroscopy of supernova remnants." New Astronomy Reviews 46, no. 8-10 (2002): 507–11. http://dx.doi.org/10.1016/s1387-6473(02)00192-6.

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Reach, William T., and Jeonghee Rho. "Infrared Spectroscopy of Molecular Supernova Remnants." Astrophysical Journal 544, no. 2 (2000): 843–58. http://dx.doi.org/10.1086/317252.

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Matheson, Thomas. "Optical Spectroscopy of Type Ia Supernovae." International Astronomical Union Colloquium 192 (2005): 161–65. http://dx.doi.org/10.1017/s0252921100009131.

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SummaryThe supernova (SN) group at the Harvard-Smithsonian Center for Astrophysics has been using the facilities of the F. L. Whipple Observatory to gather optical photometric and spectroscopic data on nearby supernovae for several years. The collection of spectra of Type Ia SNe is now large enough to allow a comprehensive analysis. I will present preliminary results from a study of a subsample of the CfA Type Ia spectroscopic database, with over 200 spectra of 31 Type Ia SNe. The SNe selected all have well-calibrated light curves and cover a wide scope of luminosity classes. The epochs of observation range from fourteen days before maximum to fifty days past maximum. All of the spectra were obtained with the same instrument on the same telescope, and were reduced using the same techniques. With such a large, homogeneous data set, the spectroscopic similarities and differences among Type Ia SNe become readily apparent.

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Caldwell, Nelson, John C. Raymond, Knox S. Long, and Myung Gyoon Lee. "Spectroscopy of Supernova Remnants and Candidates in M31." Astrophysical Journal 983, no. 2 (2025): 150. https://doi.org/10.3847/1538-4357/adbf98.

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Abstract With a star formation rate of order 0.4 M ⊙ yr−1, M31 should have a significant population of supernova remnants (SNRs) and, in fact, 156 SNRs and SNR candidates have been suggested by J. H. Lee & M. G. Lee, by searching for nebulae with elevated [S ii]/Hα ratios in narrowband images. Here, we use a combination of low- and high-resolution optical spectroscopy obtained with Hectospec on the MMT to characterize 152 of these nebulae. Of these candidates, we find 93 nebulae that have [S ii]/Hα ratios that exceed 0.4, the traditional ratio used to separate SNRs from H ii regions, strongly suggesting that at least these objects are SNRs. Our high-resolution spectroscopy reveals 108 nebulae that have velocity widths in Hα (full width at 20% peak flux) that exceed 50 km s−1, significantly larger than found in H ii regions. There are 72 objects that satisfy both tests. Here, we discuss the spectroscopic characteristics of all of the objects in our sample, and the likelihood that other objects in the sample of J. H. Lee & M. G. Lee are also SNRs, and we briefly consider confirmation by X-ray, radio, and UV observations. We also discuss several new candidates that have been identified serendipitously in the course of examining a large amount of archival Hectospec data.

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Martínez-Rodríguez, Héctor, Lluís Galbany, Carles Badenes, et al. "Recovering Lost Light: Discovery of Supernova Remnants with Integral Field Spectroscopy." Astrophysical Journal 963, no. 2 (2024): 125. http://dx.doi.org/10.3847/1538-4357/ad1bcf.

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Abstract We present results from a systematic search for broad (≥ 400 km s−1) Hα emission in integral field spectroscopy data cubes of ∼1200 nearby galaxies obtained with PMAS and MUSE. We found 19 unique regions that pass our quality cuts, four of which match the locations of previously discovered supernovae (SNe): one Type IIP and three Type IIn, including the well-known SN 2005ip. We suggest that these objects are young Supernova remnants (SNRs), with bright and broad Hα emission powered by the interaction between the SN ejecta and dense circumstellar material. The stellar ages measured at the locations of these SNR candidates are systematically lower by about 0.5 dex than those measured at the locations of core-collapse (CC) SNe, implying that their progenitors might be shorter lived and therefore more massive than a typical CCSN progenitor. The methods laid out in this work open a new window into the study of nearby SNe with integral field spectroscopy.

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Diehl, Roland, Jochen Greiner, Martin G. H. Krause, Moritz M. M. Pleintinger, and Thomas Siegert. "Gamma-ray spectroscopy of galactic nucleosynthesis." EPJ Web of Conferences 279 (2023): 02001. http://dx.doi.org/10.1051/epjconf/202327902001.

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Diffuse gamma-ray emission from the decay of radioactive 26Al is a messenger from the nucleosynthesis activity in our current-day galaxy. Because this material is attributed to ejections from massive stars and their supernovae, the gamma-ray signal includes information about nucleosynthesis in massive star interiors as it varies with evolutionary stages, and about their feedback on the surrounding interstellar medium. Our method of population synthesis of massive-star groups has been refined as a diagnostic tool for this purpose. It allows to build a bottom-up prediction of the diffuse gamma-ray sky when known massive star group distributions and theoretical models of stellar evolution and core-collapse supernova explosions are employed. We find general consistency of an origin in such massive-star groups, in particular we also find support for the clumpy distribution of such source regions across the Galaxy, and characteristics of large cavities around these. A discrepancy in the integrated 26Al gamma-ray flux is interpreted as an indication for excess 26Al emission from nearby, distributed in cavities that extend over major regions of the sky.

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31

Rose, Sam, Ryan M. Lau, Jacob E. Jencson, et al. "Investigating the Electron-capture Supernova Candidate AT 2019abn with JWST Spectroscopy." Astrophysical Journal Letters 980, no. 1 (2025): L14. https://doi.org/10.3847/2041-8213/adad61.

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Abstract The James Webb Space Telescope (JWST) has opened up a new window to study highly reddened explosive transients. We present results from late-time JWST follow-up spectroscopic observations with NIRSpec and MIRI-LRS of the intermediate-luminosity red transient (ILRT) AT 2019abn. ILRTs represent a mysterious class of transients that exhibit peak luminosities between those of classical novae and supernovae and that are known to be highly dust obscured. Similar to the prototypical examples of this class of objects, NGC 300 2008-OT and SN 2008S, AT 2019abn has an extremely red and dusty progenitor detected only in pre-explosion Spitzer/IRAC imaging at 3.6 and 4.5 μm and not in deep optical or near-infrared Hubble Space Telescope images. We find that late-time observations of AT 2019abn from NEOWISE and JWST are consistent with the late-time evolution of SN 2008S. In part because they are so obscured by dust, it is unknown what produces an ILRT, with hypotheses including high-mass stellar merger events, nonterminal stellar outbursts, and terminal supernova explosions through electron capture in super-AGB (SAGB) stars. Our JWST observations show strong mid-IR class C polycyclic aromatic hydrocarbon features at 6.3 and 8.25 μm typical of carbon-rich post-AGB sources. These features suggest that the dust around AT 2019abn is composed of carbonaceous grains, which are not typically observed around red supergiants. However, depending on the strength and temperature of hot bottom burning, SAGB stars may be expected to exhibit a carbon-rich chemistry. Thus, our JWST observations are consistent with AT 2019abn having an SAGB progenitor and exploding as an electron-capture supernova.

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32

CHEN, YANG, YANG SU, PATRICK O. SLANE, and Q. DANIEL WANG. "CHANDRA SPECTROSCOPY OF SUPERNOVA REMNANT 3C 391." Journal of The Korean Astronomical Society 38, no. 2 (2005): 211–14. http://dx.doi.org/10.5303/jkas.2005.38.2.211.

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33

Hailey, Charles J., and William W. Craig. "Spectroscopy of the supernova remnant CTB 1." Astrophysical Journal 434 (October 1994): 635. http://dx.doi.org/10.1086/174765.

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34

Thomas, R. C., P. E. Nugent, and J. C. Meza. "SYNAPPS: Data-Driven Analysis for Supernova Spectroscopy." Publications of the Astronomical Society of the Pacific 123, no. 900 (2011): 237–48. http://dx.doi.org/10.1086/658673.

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35

Dimitriadis, G., C. Rojas-Bravo, C. D. Kilpatrick, et al. "Nebular Spectroscopy of Kepler ’s Brightest Supernova." Astrophysical Journal 870, no. 2 (2019): L14. http://dx.doi.org/10.3847/2041-8213/aaf9b1.

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36

Doikov, D. N. "Positron Annihilation Spectroscopy of Young Supernova Remnants." Odessa Astronomical Publications 31 (October 15, 2018): 62–69. http://dx.doi.org/10.18524/1810-4215.2018.31.144437.

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37

Harutyunyan, A. H., P. Pfahler, A. Pastorello, et al. "ESC supernova spectroscopy of non-ESC targets." Astronomy & Astrophysics 488, no. 1 (2008): 383–99. http://dx.doi.org/10.1051/0004-6361:20078859.

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38

Kafka, Stella. "The Changing Nature of QU Carinae: SN Ia Progenitor or a Hoax?" Proceedings of the International Astronomical Union 7, S281 (2011): 149–53. http://dx.doi.org/10.1017/s1743921312014901.

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AbstractThe race to the elusive Type Ia supernovae (SNe Ia) progenitors is at its zenith, with numerous clues from SNe Ia ejecta and a dearth of observational candidates. Still, the single degenerate channel is a viable route of mass accumulation onto a white dwarf to the Chandrasekhar limit. I present long-term high resolution spectroscopy of QU Carinae, one of the most promising single degenerate SNe Ia progenitors. I discuss its highly variable nature and compare it to current scenarios for mass accumulation onto high-mass white dwarfs, eventually leading to WD detonation and to a supernova explosion.

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39

Hwang, U., R. Petre, E. Gotthelf, J. Hughes, and J. Keohane. "X-ray Spectroscopy of the Supernova Remnant N103B." Symposium - International Astronomical Union 190 (1999): 141–42. http://dx.doi.org/10.1017/s007418090011767x.

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40

Salo, Laura, Rui Zhou, Samuel Johnson, Patrick Kelly, and Galin L. Jones. "Supernova Siblings and Spectroscopic Host Galaxy Properties." Astrophysical Journal 981, no. 1 (2025): 97. https://doi.org/10.3847/1538-4357/adad60.

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Abstract Over the past century, supernova (SN) searches have detected multiple supernovae (SNe) in hundreds of individual galaxies. So-called SN siblings discovered in the same galaxy present an opportunity to constrain the dependence of the properties of SNe on those of their host galaxies. To investigate whether there is a connection between sibling SNe in galaxies that have hosted multiple SNe and the properties of galaxies, we have acquired integrated optical spectroscopy of 59 galaxies with multiple core-collapse SNe. Perhaps surprisingly, a strong majority of host galaxy spectra fall within the composite region of the Baldwin–Phillips–Terlevich (BPT) diagram. We find a statistically significant difference (Kolmogorov–Smirnov test p-value = 0.044) between the distributions of the [N ii] λ6583/Hα of galaxies that have hosted a majority of SNe Ibc and those that have hosted a majority of Type II supernovae (SNe II), where the majority of Type Ibc supernovae (SNe Ibc) galaxies have, on average, higher ratios. The difference between the distributions of [N ii] λ6583/Hα may arise from either increased contribution from active galactic nuclei or low-ionization nuclear emission-line regions in SNe Ibc host galaxies, greater metallicity for SNe Ibc host galaxies, or both. When comparing the inferred oxygen abundance and the ionization parameter for the galaxies in the star-forming region on the BPT diagram, we find statistically significant differences between the distributions for SNe Ibc hosts and SNe II hosts (p = 0.008 and p = 0.001, respectively), as well as SNe Ib hosts and SNe II hosts (p = 0.030 and p = 0.006, respectively). We also compare the Hα equivalent width distributions, also integrated across the galaxies, and find no significant difference.

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41

Dastidar, Raya, Kuntal Misra, Mridweeka Singh, et al. "SN 2016B a.k.a. ASASSN-16ab: a transitional Type II supernova." Monthly Notices of the Royal Astronomical Society 486, no. 2 (2019): 2850–72. http://dx.doi.org/10.1093/mnras/stz949.

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Abstract We present photometry, polarimetry, and spectroscopy of the Type II supernova ASASSN-16ab/SN 2016B in PGC 037392. The photometric and spectroscopic follow-up commenced about 2 weeks after shock breakout and continued until nearly 6 months. The light curve of SN 2016B exhibits intermediate properties between those of Type IIP and IIL. The early decline is steep (1.68 ± 0.10 mag 100 d−1), followed by a shallower plateau phase (0.47 ± 0.24 mag 100 d−1). The optically thick phase lasts for 118 d, similar to Type IIP. The 56Ni mass estimated from the radioactive tail of the bolometric light curve is 0.082 ± 0.019 M⊙. High-velocity component contributing to the absorption trough of H α and H β in the photospheric spectra are identified from the spectral modelling from about 57–97 d after the outburst, suggesting a possible SN ejecta and circumstellar material interaction. Such high-velocity features are common in the spectra of Type IIL supernovae. By modelling the true bolometric light curve of SN 2016B, we estimated a total ejected mass of ∼15 M⊙, kinetic energy of ∼1.4 foe, and an initial radius of ∼400 R⊙.

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Petre, R., P. J. Serlemitsos, F. E. Marshall, et al. "BBXRT Observations of Supernova Remnants." Highlights of Astronomy 9 (1992): 229–33. http://dx.doi.org/10.1017/s1539299600008972.

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AbstractThe BBXRT observed nine supernova remnants during its nine-day flight. We present preliminary results from some of these observations, emphasizing the ability of BBXRT to perform spatially resolved spectroscopy. The improved spectral resolution and efficiency over previous instruments makes possible measurements of previously undetectable lines, and the broad bandpass allows simultaneous measurement of lines from oxygen through iron.

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43

Kwok, Lindsey A., Marc Williamson, Saurabh W. Jha, et al. "Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad." Astrophysical Journal 937, no. 1 (2022): 40. http://dx.doi.org/10.3847/1538-4357/ac8989.

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Abstract Few published ultraviolet (UV) spectra exist for stripped-envelope supernovae and none to date for broad-lined Type Ic supernovae (SNe Ic-bl). These objects have extremely high ejecta velocities and are the only supernova type directly linked to gamma-ray bursts (GRBs). Here we present two epochs of HST/STIS spectra of the SN Ic-bl 2014ad, the first UV spectra for this class. We supplement this with 26 new epochs of ground-based optical spectra, augmenting a rich spectral time series. The UV spectra do not show strong features and are consistent with broadened versions of other SN Ic spectra observed in the UV. We measure Fe ii 5169 Å velocities and show that SN 2014ad has even higher ejecta velocities than most SNe Ic both with and without observed GRBs. We construct models of the SN 2014ad UV+optical spectra using tardis, a 1D Monte Carlo radiative-transfer spectral synthesis code. The models fit the data well at multiple epochs in the optical but underestimate the flux in the UV, likely due to simplifying assumptions. We find that high densities at high velocities are needed to reproduce the spectra, with ∼3 M ⊙ of material at v > 22,000 km s−1, assuming spherical symmetry. Our nebular line fits suggest a steep density profile at low velocities. Together, these results imply a higher total ejecta mass than estimated from previous light-curve analysis and expected from theory. This may be reconciled by a flattening of the density profile at low velocity and extra emission near the center of the ejecta.

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44

Parrag, Eleonora, Cosimo Inserra, Steve Schulze, et al. "SN 2019hcc: a Type II supernova displaying early O ii lines." Monthly Notices of the Royal Astronomical Society 506, no. 4 (2021): 4819–40. http://dx.doi.org/10.1093/mnras/stab2074.

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ABSTRACT We present optical spectroscopy together with ultraviolet, optical, and near-infrared photometry of SN 2019hcc, which resides in a host galaxy at redshift 0.044, displaying a sub-solar metallicity. The supernova spectrum near peak epoch shows a ‘w’ shape at around 4000 Å which is usually associated with O ii lines and is typical of Type I superluminous supernovae. SN 2019hcc post-peak spectra show a well-developed H α P-Cygni profile from 19 d past maximum and its light curve, in terms of its absolute peak luminosity and evolution, resembles that of a fast-declining Hydrogen-rich supernova (SN IIL). The object does not show any unambiguous sign of interaction as there is no evidence of narrow lines in the spectra or undulations in the light curve. Our tardis spectral modelling of the first spectrum shows that carbon, nitrogen, and oxygen (CNO) at 19 000 K reproduce the ‘w’ shape and suggests that a combination of non-thermally excited CNO and metal lines at 8000 K could reproduce the feature seen at 4000 Å. The Bolometric light-curve modelling reveals that SN 2019hcc could be fit with a magnetar model, showing a relatively strong magnetic field (B &gt; 3 × 1014 G), which matches the peak luminosity and rise time without powering up the light curve to superluminous luminosities. The high-energy photons produced by the magnetar would then be responsible for the detected O ii lines. As a consequence, SN 2019hcc shows that a ‘w’ shape profile at around 4000 Å, usually attributed to O ii, is not only shown in superluminous supernovae and hence it should not be treated as the sole evidence of the belonging to such a supernova type.

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45

Long, Knox S., William P. Blair, Dan Milisavljevic, John C. Raymond, and P. Frank Winkler. "MMT Spectroscopy of Supernova Remnant Candidates in M33." Astrophysical Journal 855, no. 2 (2018): 140. http://dx.doi.org/10.3847/1538-4357/aaac7e.

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46

KOO, BON-CHUL, and YONG-HYUN LEE. "NEAR-INFRARED SPECTROSCOPY OF YOUNG GALACTIC SUPERNOVA REMNANTS." Publications of The Korean Astronomical Society 30, no. 2 (2015): 145–48. http://dx.doi.org/10.5303/pkas.2015.30.2.145.

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47

Anupama, G. C., T. Sivarani, and G. Pandey. "Early time optical spectroscopy of supernova SN 1998S." Astronomy & Astrophysics 367, no. 2 (2001): 506–12. http://dx.doi.org/10.1051/0004-6361:20000427.

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48

Graham, James R., Gillian S. Wright, and Andrew J. Longmore. "Infrared spectroscopy of the supernova remnant IC 443." Astrophysical Journal 313 (February 1987): 847. http://dx.doi.org/10.1086/165023.

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49

Maeda, K., K. Kawabata, P. A. Mazzali, et al. "Asphericity in Supernova Explosions from Late-Time Spectroscopy." Science 319, no. 5867 (2008): 1220–23. http://dx.doi.org/10.1126/science.1149437.

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50

Galbany, Lluís, Vallery Stanishev, and Ana Mourão. "Using the environment to understand supernova properties." Proceedings of the International Astronomical Union 9, S296 (2013): 350–51. http://dx.doi.org/10.1017/s1743921313009770.

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AbstractWe present three studies that use supernova (SN) environments within host galaxies (HGs) to constrain SNe properties. These studies are ordered from an indirect approximation to a direct determination of the environmental parameters of the SN. We find correlations between the galactocentric distance and several parameters measured from both the SN light-curve (LC) and the host galaxy spectroscopy. We are able to recover and strength previous results pointing to a sequence on the progenitor mass of different SN types. We also confirm no significant difference in the elemental abundances of the environment where different SN types exploded, measured with a more powerful technique such as Integral Field Spectroscopy (IFS).

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