Hubble Space Telescope Images and Spectra of the Remnant of SN 1885 in M31

Fesen, Robert A.; Gerardy, Christopher L.; McLin, K.; Hamilton, A.

doi:10.1086/306938

Cited by 21 publications

(68 citation statements)

References 30 publications

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“…12 we see a very dim X-ray emission at the position of SN 1885A (Fesen et al 1999), which is not included in the catalogue. Source properties were extracted from a circular region with a radius of 0.7 (see estimated extent in Sjouwerman & Dickel 2001) from the merged high-resolution image at the position of SN 1885A.…”

Section: Supernova Remnantsmentioning

confidence: 91%

“…12. Contour plots of the logarithmically scaled merged HRC-I images with dashed circular regions at the radio positions with approximate radio radii (Fesen et al 1999;Sjouwerman & Dickel 2001) of the known supernova remnants within 90 of the center of M 31. The images are smoothed with a Gaussian function of 7-pixel FWHM and contour levels are at 0.53, 0.56, 0.6, and 0.7 counts per pixel.…”

Section: Supernova Remnantsmentioning

confidence: 99%

See 1 more Smart Citation

X-ray source variability study of the M 31 central field usingChandraHRC-I

Pietsch¹,

Henze²,

Haberl³

et al. 2013

A&A

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Context. The central field of the Andromeda galaxy (M 31) was monitored from 2006 to 2012 using the Chandra HRC-I detector (about 0.1−10 keV energy range) with the main aim of detecting X-rays from optical novae. We present a systematic analysis of all X-ray sources found in the 41 nova monitoring observations, along with 23 M 31 central field HRC-I observations available from the Chandra data archive starting in December 1999. Aims. Based on these observations, we studied the X-ray long-term variability of the source population and especially of X-ray binaries in M 31. Methods. We created a catalogue of sources detected in the 64 available observations that adds up to a total exposure time of about 1 Ms. To study the variability, we developed a processing pipeline to derive long-term Chandra HRC-I light curves for each source over the 13 years of observations. We also searched for extended X-ray sources in the merged images.Results. We present a point-source catalogue containing 318 X-ray sources with detailed long-term variability information, 28 of which are published for the first time. The spatial and temporal resolution of the catalogue allows us to classify 115 X-ray binary candidates showing high X-ray variability or even outbursts, as well as 14 globular cluster X-ray binary candidates showing no significant variability. The analysis may suggest that outburst sources are less frequent in globular clusters than in the field of M 31. We detected seven supernova remnants, one of which is a new candidate, and also resolved the first X-rays from a known radio supernova remnant. In addition to 33 known optical nova/X-ray source correlations, we discovered one previously unknown super-soft X-ray outburst and several new nova candidates. Conclusions. The catalogue contains a large sample of detailed long-term X-ray light curves in the M 31 central field, which helps in understanding the X-ray population of our neighbouring spiral galaxy M 31.

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Section: Supernova Remnantsmentioning

confidence: 91%

Section: Supernova Remnantsmentioning

confidence: 99%

X-ray source variability study of the M 31 central field usingChandraHRC-I

Pietsch¹,

Henze²,

Haberl³

et al. 2013

A&A

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“…The remnant is still in free expansion, and has reached a diameter of 0.7-0.8 arcsec, implying an outer-edge ejecta velocity of ∼12 500 km s −1 (Fesen et al, 1999). The strongest absorption (down to ∼ 20% transmission) is observed in the Ca II H&K resonance lines, where the remnant looks nearly spherical on global scales (Fesen et al, 1999, 2015). Other detected absorption lines are from Ca I, Fe I and Fe II.…”

Section: The Remnant Of Sn 1885amentioning

confidence: 97%

“…All previous searches for emission lines, starting already with Walter Baade in the 1940s (Osterbrock, 2001), had failed. Subsequent HST imaging and spectroscopy of the remnant (Fesen et al, 1999(Fesen et al, , 2007(Fesen et al, , 2015Hamilton & Fesen, 2000) allowed a much more detailed study of its size, composition and geometry. The remnant is still in free expansion, and has reached a diameter of 0.7-0.8 arcsec, implying an outer-edge ejecta velocity of ∼12 500 km s −1 (Fesen et al, 1999).…”

Section: The Remnant Of Sn 1885amentioning

confidence: 99%

The Extremes of Thermonuclear Supernovae

Taubenberger¹

2016

Handbook of Supernovae

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The majority of thermonuclear explosions in the Universe seem to proceed in a rather standardised way, as explosions of carbon-oxygen (CO) white dwarfs in binary systems, leading to 'normal' Type Ia supernovae (SNe Ia). However, over the years a number of objects have been found which deviate from normal SNe Ia in their observational properties, and which require different and not seldom more extreme progenitor systems. While the 'traditional' classes of peculiar SNe Ia -luminous '91T-like' and faint '91bg-like' objects -have been known since the early 1990s, other classes of even more unusual transients have only been established 20 years later, fostered by the advent of new wide-field SN surveys such as the Palomar Transient Factory. These include the faint but slowly declining '02es-like' SNe, 'Ca-rich' transients residing in the luminosity gap between classical novae and supernovae, extremely short-lived, fast-declining transients, and the very luminous so-called 'super-Chandrasekhar' SNe Ia. Not all of them are necessarily thermonuclear explosions, but there are good arguments in favour of a thermonuclear origin for most of them. The aim of this chapter is to provide an overview of the zoo of potentially thermonuclear transients, reviewing their observational characteristics and discussing possible explosion scenarios.

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“…There is also one extragalactic SNR detected in absorption lines: the remnant of SN 1885 in M 31. It was first detected by groundbased imaging in Fe I 3860 Å band against the M 31 bulge (Fesen et al 1989) and afterwards by HST imaging and spectroscopy (Fesen et al 1999). The optical spectrum of this SNR contains strong Fe I, Ca II, and Ca I broad resonance absorption lines produced by the unshocked ejecta.…”

Section: Introductionmentioning

confidence: 99%

Search for broad absorption lines in spectra of stars in the field of supernova remnant RX J0852.0-4622 (Vela Jr.)

Iyudin

Pakhomov

Чугай

et al. 2010

A&A

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Aims. Supernova remnant (SNR) RX J0852.0-4622 is one of the youngest and is most likely the closest among known Galactic SNRs. It was detected in X-rays, the 44 Ti γ-line, and radio. We obtain and analyze medium-resolution spectra of 14 stars in the direction towards the SNR RX J0852.0-4622 in an attempt to detect broad absorption lines of unshocked ejecta against background stars. Methods. Spectral synthesis is performed for all the stars in the wavelength range of 3740−4020 Å to extract the broad absorption lines of Ca II related to the SNR RX J0852.0-4622. Results. We do not detect any broad absorption line and place a 3σ upper limit on the relative depths of <0.04 for the broad Ca II absorption produced by the SNR. We detect narrow low and high velocity absorption components of Ca II. High velocity |V LSR | ∼ 100−140 km s −1 components are attributed to radiative shocks in clouds engulfed by the old Vela SNR. The upper limit to the absorption line strength combined with the width and flux of the 44 Ti γ-ray line 1.16 MeV lead us to conclude that SNR RX J0852.0-4622 was probably produced by an energetic SN Ic explosion.

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Hubble Space Telescope Images and Spectra of the Remnant of SN 1885 in M31

Cited by 21 publications

References 30 publications

X-ray source variability study of the M 31 central field usingChandraHRC-I

X-ray source variability study of the M 31 central field usingChandraHRC-I

The Extremes of Thermonuclear Supernovae

Search for broad absorption lines in spectra of stars in the field of supernova remnant RX J0852.0-4622 (Vela Jr.)

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