EARLY OBSERVATIONS AND ANALYSIS OF THE TYPE Ia SN 2014J IN M82

Marion, G. H.; Sand, David J.; Hsiao, E. Y.; Banerjee, D. P. K.; Valenti, S.; Stritzinger, M. D.; Vinkó, J.; Joshi, Vishal; Venkataraman, V.; Ashok, N. M.; Amanullah, R.; Binzel, Richard P.; Bochanski, John J.; Bryngelson, Ginger; Burns, C. R.; Drozdov, Dina; Fieber-Beyer, S. K.; Graham, M. L.; Howell, D. A.; Johansson, Joel; Kirshner, R.; Milne, Peter; Parrent, J.; Silverman, J. M.; Vervack, R. J.; Wheeler, J. C.

doi:10.1088/0004-637x/798/1/39

Cited by 71 publications

(126 citation statements)

References 73 publications

Supporting

Mentioning

108

Contrasting

Order By: Relevance

“…4.4). We note that no LVG SNe in Benetti et al (2005) have v SiII ≥ 11 000 km s −1 around B-band maximum, but v SiII ≈ 11 750 km s −1 for SN 2014J at that epoch (Ashall et al 2014;Kawabata et al 2014;Marion et al 2015).…”

Section: Broad Lines Of Sn 2011fe and 2014jmentioning

confidence: 69%

See 1 more Smart Citation

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

Lundqvist

Nyholm

Taddia

et al. 2015

A&A

Self Cite

121

View full text Add to dashboard Cite

Aims. This study aims at constraining the origin of the nearby Type Ia supernovae (SNe), 2011fe and 2014J. The two most favoured scenarios for triggering the explosion of the white dwarf supernova progenitor is either mass loss from a non-degenerate companion or merger with another white dwarf. In the former, there could be a significant amount of leftover material from the companion at the centre of the supernova. Detecting such material would therefore favour the single-degenerate scenario. Methods. The left-over material from a possible non-degenerate companion can reveal itself after about one year, and in this study such material was searched for in the spectra of SN 2011fe (at 294 days after the explosion) using the Large Binocular Telescope and for SN 2014J using the Nordic Optical Telescope (315 days past explosion). The observations were interpreted using numerical models simulating the expected line emission from ablated material from the companion star. λλ7291, 7324 could be traced for in any of the two supernovae. When systematic uncertainties are included, the limits on hydrogen-rich ablated gas are 0.003 M in SN 2011fe and 0.0085 M in SN 2014J, where the limit for SN 2014J is the second lowest ever, and the limit for SN 2011fe is a revision of a previous limit. Limits are also put on heliumrich ablated gas, and here limits from [O I] λ6300 provide the upper mass limits 0.002 M and 0.005 M for SNe 2011fe and 2014J, respectively. These numbers are used in conjunction with other data to argue that these supernovae can stem from double-degenerate systems or from single-degenerate systems with a spun-up/spun-down super-Chandrasekhar white dwarf. For SN 2011fe, other types of hydrogen-rich donors can very likely be ruled out, whereas a main-sequence donor system with large intrinsic separation is still possible for SN 2014J. Helium-rich donor systems cannot be ruled out for any of the two supernovae, but the expected short delay time for such progenitors makes this possibility less likely, especially for SN 2011fe. Published data for SNe 1998bu, 2000cx, 2001el, 2005am, and 2005cf are used to constrain their origin. We emphasise that the results of this study depend on the sought-after lines emerging unattenuated from the central regions of the nebula. Detailed radiative transfer calculations with longer line lists than are presently used are needed to confirm that this is, in fact, true. Finally, the broad lines of SNe 2011fe and 2014J are discussed, and it is found that the [Ni II] λ7378 emission is redshifted by ∼+1300 km s −1 , as opposed to the known blueshift of ∼−1100 km s −1 for SN 2011fe. [Fe II] λ7155 is also redshifted in SN 2014J. SN 2014J belongs to a minority of SNe Ia that both have a nebular redshift of [Fe II] λ7155 and [Ni II] λ7378, and a slow decline of the Si II λ6355 absorption trough just after B-band maximum.

show abstract

Section: Broad Lines Of Sn 2011fe and 2014jmentioning

confidence: 69%

“…The decline rate in this velocity (v SiII ) is calledv Si , and Maeda et al (2010a) Consulting the results of Kawabata et al (2014) and Marion et al (2015) for SN 2014J, we find thatv Si ∼55 km s…”

Section: Broad Lines Of Sn 2011fe and 2014jmentioning

confidence: 73%

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

Lundqvist

Nyholm

Taddia

et al. 2015

A&A

Self Cite

121

View full text Add to dashboard Cite

show abstract

“…Its expansion velocity decreases from 24,000 km/s in our first spectrum down to about 20,000 km/s in the spectrum 6 days later. In their study of near infrared spectra of SN 2014J, Marion, G. H. et al, (2015) found a similar behaviour for the Ca II IR triplet expansion velocities. They measured values for the high expansion velocity feature between 26,000 km/s and 20,000 km/s.…”

Section: Expansion Velocities Of Si II and Ca Iimentioning

confidence: 67%

Time series of high-resolution spectra of SN 2014J observed with the TIGRE telescope

Jack¹,

Mittag²,

Schröder³

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present a time series of high resolution spectra of the Type Ia supernova 2014J, which exploded in the nearby galaxy M82. The spectra were obtained with the HEROŚ echelle spectrograph installed at the 1.2 m TIGRE telescope. We present a series of 33 spectra with a resolution of R ≈ 20, 000, which covers the important bright phases in the evolution of SN 2014J during the period from January 24 to April 1 of 2014. The spectral evolution of SN 2014J is derived empirically. The expansion velocities of the Si II P-Cygni features were measured and show the expected decreasing behaviour, beginning with a high velocity of 14,000 km/s on January 24. The Ca II infrared triplet feature shows a high velocity component with expansion velocities of > 20, 000 km/s during the early evolution apart from the normal component showing similar velocities as Si II. Further broad P-Cygni profiles are exhibited by the principal lines of Ca II, Mg II and Fe II. The TIGRE SN 2014J spectra also resolve several very sharp Na I D doublet absorption components. Our analysis suggests interesting substructures in the interstellar medium of the host galaxy M82, as well as in our Milky Way, confirming other work on this SN. We were able to identify the interstellar absorption of M82 in the lines of Ca II H & K at 3933 and 3968Å as well as K I at 7664 and 7698Å. Furthermore, we confirm several Diffuse Interstellar Bands, at wavelengths of 6196, 6283, 6376, 6379 and 6613Å and give their measured equivalent widths.

show abstract

“…This is not in contradiction, since strong resonance lines can extend to high velocities at early times, when the density is high in the outer ejecta. (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 .…”

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: 89%

“…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).…”

mentioning

confidence: 99%

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.

View full text Add to dashboard Cite

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.

show abstract

EARLY OBSERVATIONS AND ANALYSIS OF THE TYPE Ia SN 2014J IN M82

Cited by 71 publications

References 73 publications

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

Time series of high-resolution spectra of SN 2014J observed with the TIGRE telescope

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

Contact Info

Product

Resources

About