The Rise of Sn 2014j in the Nearby Galaxy M82

Goobar, A.; Johansson, Joel; Amanullah, R.; Cao, Y.; Perley, D.; Kasliwal, M. M.; Ferretti, R.; Nugent, P.; Harris, Chelsea E.; Gal‐Yam, A.; Ofek, E. O.; Tendulkar, Shriharsh P.; Dennefeld, M.; Valenti, S.; Arcavi, I.; Banerjee, D. P. K.; Venkataraman, V.; Joshi, Vishal; Ashok, N. M.; Cenko, S. Bradley; Diaz, R. F.; Fremling, C.; Horesh, A.; Howell, D. A.; Kulkarni, S. R.; Papadogiannakis, S.; Petrushevska, T.; Sand, David J.; Sollerman, J.; Stanishev, V.; Bloom, J.; Surace, J.; Dupuy, Trent J.; Liu, Mengmeng

doi:10.1088/2041-8205/784/1/l12

Cited by 125 publications

(177 citation statements)

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“…From bluer wavelengths we see, as pointed out by previous works, that the SN is heavily reddened by dust in the host galaxy. Although the spectra shown in the Figure has not been corrected for Milky Way (MW) and host galaxy extinction, the spectral parameters described below have been measured after applying these corrections using a Fitzpatrick 1999 law, for both the MW using the dust maps of Schlafly & Finkbeiner (2011) assuming an RV = 3.1, and for the host galaxy with the reported values of E(B − V ) = 1.2 and RV = 1.4 from Goobar et al (2014).…”

Section: Spectral Characterizationmentioning

confidence: 99%

SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

Galbany

Moreno-Raya

Ruiz‐Lapuente

et al. 2016

Mon. Not. R. Astron. Soc.

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We present the intensive spectroscopic follow up of the type Ia supernova (SN Ia) 2014J in the starburst galaxy M82. Twenty-seven optical spectra have been acquired from January 22 nd to September 1 st 2014 with the Isaac Newton (INT) and William Herschel (WHT) Telescopes. After correcting the observations for the recession velocity of M82 and for Milky Way and host galaxy extinction, we measured expansion velocities from spectral line blueshifts and pseudo-equivalent width of the strongest features in the spectra, which gives an idea on how elements are distributed within the ejecta. We position SN 2014J in the Benetti (2005)

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Section: Spectral Characterizationmentioning

confidence: 99%

SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

Galbany

Moreno-Raya

Ruiz‐Lapuente

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Recent examples of early-observed and well-studied SNeIa include SN2009ig (Foley et al 2012), SN2011fe Nugent et al 2011), SN2012cg (Silverman et al 2012b), SN2013dy , iPTF13ebh (Hsiao et al 2015), SN2014J (Goobar et al 2014;Zheng et al 2014;Graham et al 2015), and ASASSN-14lp (Shappee et al 2016); like SN2016coj discussed here, they were either discovered or detected shortly after exploding.…”

Section: Introductionmentioning

confidence: 58%

Discovery and Follow-up Observations of the Young Type Ia Supernova 2016coj

Zheng

Filippenko

Mauerhan

et al. 2017

ApJ

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The TypeIa supernova (SN Ia) 2016coj in NGC4125 (redshift z=0.00452±0.00006) was discovered by the Lick Observatory Supernova Search 4.9 days after the fitted first-light time (FFLT; 11.1 days before B-band maximum). Our first detection (prediscovery) is merely 0.6±0.5 days after the FFLT, making SN2016coj one of the earliest known detections of an SNIa. A spectrum was taken only 3.7 hr after discovery (5.0 days after the FFLT) and classified as a normal SNIa. We performed high-quality photometry, low-and high-resolution spectroscopy, and spectropolarimetry, finding that SN2016coj is a spectroscopically normal SNIa, but the velocity of Si II λ6355 around peak brightness (∼12,600 km s 1 -) is a bit higher than that of typical normal SNe. The Si II λ6355 velocity evolution can be well fit by a broken-power-law function for up to a month after the FFLT. SN2016coj has a normal peak luminosity (M 18.9 0.2 B » - mag), and it reaches a B-band maximum ∼16.0days after the FFLT. We estimate there to be low host-galaxy extinction based on the absence of Na ID absorption lines in our low-and high-resolution spectra. The spectropolarimetric data exhibit weak polarization in the continuum, but the Si II line polarization is quite strong (∼0.9%±0.1%) at peak brightness.

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“…(Ashall et al 2014;Kawabata et al 2014;Tsvetkov et al 2014;Marion et al 2015); SN 2011fe: 1.11 ± 0.07 (Richmond & Smith 2012;Pereira et al 2013;McClelland et al 2013;Tammann & Reindl 2013) and different line and photospheric velocities, up to 1500 kms −1 around maximum, as shown in Fig 5. Neither SN 2011fe nor SN 2014J show traces of a single degenerate companion (Lundqvist et al 2015, but see also Graham et al 2015) favouring, in principle, the double degenerate scenario (see also Soker, García-Berro & Althaus 2014;Soker 2015). SN 2014J is highly reddened E(B − V) = 1.2 (Goobar et al 2014), while SN 2011fe is not, E(B − V) = 0.03 . Observed properties of both supernovae can be explained by the delayed-detonation explosion of a carbonoxygen white dwarf (WD) with a mass close to the Chandrasekhar mass.…”

Section: P H Oto S P H E R I C V E L O C I T Y C O M Pa R I S O N Smentioning

confidence: 93%

“…modern SN Ia, SN 2014J has been extremely well observed: in γ -rays (Churazov et al 2014;Diehl et al 2014), X-rays (Margutti et al 2014), by Hubble Space Telescope Kelly et al 2014), optical (Amanullah et al 2014;Ashall et al 2014;Goobar et al 2014;Nielsen et al 2014) at high resolution (Welty et al 2014;Graham et al 2015;Jack, Baron & Hauschildt 2015;Ritchey et al 2015), near-infrared (near-IR; Friesen et al 2014;Marion et al 2015), mid-IR (Johansson et al 2014;Telesco et al 2015), polarimetry (Kawabata et al 2014), with rapid photometry (Siverd et al 2015), and in radio (Pérez-Torres et al 2014).…”

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confidence: 99%

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Supernova 2014J at M82 – II. Direct analysis of a middle-class Type Ia supernova

Vallely

Moreno-Raya

Baron

et al. 2016

Mon. Not. R. Astron. Soc.

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We analyze a time series of optical spectra of SN 2014J from almost two weeks prior to maximum to nearly four months after maximum. We perform our analysis using the SYNOW code, which is well suited to track the distribution of the ions with velocity in the ejecta. We show that almost all of the spectral features during the entire epoch can be identified with permitted transitions of the common ions found in normal SNe Ia in agreement with previous studies.We show that 2014J is a relatively normal SN Ia. At early times the spectral features are dominated by Si II, S II, Mg II, and Ca II. These ions persist to maximum light with the appearance of Na I and Mg I. At later times iron-group elements also appear, as expected in the stratified abundance model of the formation of normal type Ia SNe.We do not find significant spectroscopic evidence for oxygen, until 100 days after maximum light. The +100 day identification of oxygen is tentative, and would imply significant mixing of unburned or only slight processed elements down to a velocity of 6,000 km s −1 . Our results are in relatively good agreement with other analyses in the IR. We briefly compare SN 2011fe to SN 2014J and conclude that the differences could be due to different central densities at ignition or differences in the C/O ratio of the progenitors.

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The Rise of Sn 2014j in the Nearby Galaxy M82

Abstract: We report on the discovery of SN 2014J in the nearby galaxy M 82. Given its

Cited by 125 publications

References 42 publications

SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

Discovery and Follow-up Observations of the Young Type Ia Supernova 2016coj

Supernova 2014J at M82 – II. Direct analysis of a middle-class Type Ia supernova

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