Luminous M giants in the bulge of M31

Rich, R. Michael; Mould, Jeremy; Picard, A.; Frogel, J. A.; Davies, Richard

doi:10.1086/185455

Cited by 86 publications

(109 citation statements)

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“…By placing V1309 Sco at the distance of 8 kpc and assuming m V (max) = 7.9 mag (see Fig. 1), we derive the upper limit of M V = −8.3 mag, which is almost 2 mag fainter than the absolute magnitude derived for V838 Mon (Sparks et al 2008) and M31-RV (Rich et al 1989). However, should the red nova be explained by stellar merging phenomena, the maximum luminosity is not necessarily a stringent constraint.…”

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confidence: 82%

“…They have never shown evidence either of high ionization potential element emission lines nor they entered the nebular or coronal phases typically observed in CNe (e.g. Munari et al 2007;Barsukova et al 2007;Rushton et al 2005;Banerjee & Ashok 2002;Rich et al 1989;Mould et al 1990;Martini et al 1999). Forbidden transitions from [OI] and [FeII] have been reported in the late spectra of V838 Mon (>+7 months since outburst, Wagner & Starrfield 2002;Munari et al 2007;Kaminski et al 2009) and V4332 Sgr (≥+5 months since outburst, Martini et al 1999).…”

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confidence: 99%

“…Forbidden transitions from [OI] and [FeII] have been reported in the late spectra of V838 Mon (>+7 months since outburst, Wagner & Starrfield 2002;Munari et al 2007;Kaminski et al 2009) and V4332 Sgr (≥+5 months since outburst, Martini et al 1999). Large luminosities have been derived for M31-RV (M bol = −10 mag, Rich et al 1989; see also Mould et al 1990) and V838 Mon (M V = −9.8 mag, Sparks et al 2008; see also Bond et al 2003;Tylenda 2004;, and reference therein; Soker & Tylenda 2003;; while the distance of V4332 Sgr is uncertain. In addition, the outburst light curve of the 3 objects differ in their time scale and (within the number of data points available for each of them) morphology, though Munari et al (2007) have noted that they are "remarkably similar" once scaled by the time of their optical brightness free-fall.…”

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confidence: 99%

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The peculiar nova V1309 Scorpii/nova Scorpii 2008

Mason¹,

Diaz²,

Williams³

et al. 2010

A&A

116

157

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Aims. Nova Scorpii 2008 was the target of our Director Discretionary Time proposal at VLT+UVES in order to study the evolution, origin and abundances of the heavy-element absorption system recently discovered in 80% of classical novae in outburst. Methods. The early decline of nova Scorpii 2008 was monitored with high resolution echelle spectroscopy at 5 different epochs. The analysis of the absorption and the emission lines show many unusual characteristics. Results. Nova Scorpii 2008 is confirmed to differ from a common classical nova as well as a symbiotic recurrent nova, and it shows characteristics which are common to the so called, yet debated, red-novae. The origin of this new nova remains uncertain.

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confidence: 82%

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confidence: 99%

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confidence: 99%

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The peculiar nova V1309 Scorpii/nova Scorpii 2008

Mason¹,

Diaz²,

Williams³

et al. 2010

A&A

116

157

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“…Soker & Tylenda (2003) proposed a stellar merging event (see also Kato 2003), but this would seem untenable in view of the apparent recurrent ejection episodes evidenced by the HST imagery (Bond et al 2003). The similarities between V838 Mon's behavior and that of M31 RV (Rich et al 1989), V4334 Sgr (Evans, Smalley, & Kimeswenger 2002), and V4332 Sgr (Martini et al 1999) have been noted by several groups (Wagner et al 2002b;Kimeswenger et al 2002;Munari et al 2002b;Bond et al 2003). Retter & Marom (2003) suggest that the object's observed behavior could be explained by an expanding central red giant that enveloped three relatively massive planets in close orbits.…”

Section: Introductionmentioning

confidence: 98%

0.8–13 Micron Spectroscopy of V838 Monocerotis and a Model for Its Emission

Lynch

Rudy

Russell

et al. 2004

ApJ

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We report on the results of a number of infrared spectra (0.8-2.5, 2.1-4.6, and 3-14 m) of V838 Monocerotis, taken from a short time after discovery in 2002 January to about 14 months later, in early 2003. The spectrum evolved dramatically, changing from a quasi-photospheric stellar spectrum with weak atomic emission lines (some with P Cygni profiles) to one showing a wide range of deep absorption features indicative of a cool, extended atmosphere with a circumstellar dust shell. The early spectra showed lines of s-process elements, such as Sr ii and Ba i. The later spectra showed absorption by gaseous H 2 O, CO, AlO, TiO, SiO, SO 2 , OH, VO, and SH, as well as a complex of emission near 10 m reminiscent of silicate emission, with a central absorbing feature at 10:3 m. Thus, V838 Mon appears to be oxygen-rich. A simple, spherically symmetric model of the system involving a central star with a two-component expanding circumstellar shell is presented that is able to explain the major molecular features and spectral energy distribution in the object's late stages. The derived shell mass and distance are 0.04 M and 9.2 kpc, respectively.

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“…The modern observational history of these events goes back to 1988, when the transient M31-RV was detected by Rich et al (1989) as an M0 supergiant variable with peak absolute M bol ∼ −10. A similar outburst in the Milky Way was observed in 1994, when V4332 Sgr changed its spectrum from K3 to M8-9 Table 4 is available in electronic form at http://www.aanda.org during a three-month period (Martini et al 1999).…”

Section: Introductionmentioning

confidence: 99%

The January 2015 outburst of a red nova in M 31

Kurtenkov

Pessev

Tomov

et al. 2015

A&A

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Context. M31N 2015M31N -01a (or M31LRN 2015 is a red nova that erupted in January 2015 -the first event of this kind observed in M 31 since 1988. Very few similar events have been confirmed as of 2015. Most of them are considered to be products of stellar mergers. Aims. Results of an extensive optical monitoring of the transient in the period January-March 2015 are presented. Methods. Eight optical telescopes were used for imaging. Spectra were obtained on the Large Altazimuth Telescope (BTA), the Gran Telecsopio Canarias (GTC) and the Rozhen 2 m telescope. Results. We present a highly accurate 70 d light curve and astrometry with a 0.05 uncertainty. The colour indices reached a minimum of 2−3 d before peak brightness and rapidly increased afterwards. The spectral type changed from F5I to F0I in 6 d before the maximum and then to K3I in the next 30 d. The luminosity of the transient was estimated to be 8.7 +3.3 −2.2 × 10 5 L during the optical maximum. Conclusions. Both the photometric and the spectroscopic results confirm that the object is a red nova, similar to V838 Monocerotis.

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Luminous M giants in the bulge of M31

Cited by 86 publications

References 0 publications

The peculiar nova V1309 Scorpii/nova Scorpii 2008

The peculiar nova V1309 Scorpii/nova Scorpii 2008

0.8–13 Micron Spectroscopy of V838 Monocerotis and a Model for Its Emission

The January 2015 outburst of a red nova in M 31

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