Near-Infrared Spectroscopy of Nova Sagittarius 1999 (V4444 Sagittarii)

Venturini, C. C.; Rudy, R. J.; Lynch, D. K.; Mazuk, S.; Puetter, R. C.

doi:10.1086/343832

Cited by 14 publications

(18 citation statements)

References 26 publications

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“…Fig. 10.-CI Aql's early spectra are similar to those seen previously in V4642 Sgr = Nova Sagittarii 2000 , V1494 Aql = Nova Aquilae 1999#2 (Venturini et al 2000;Rudy et al 2001), and V4633 Sgr = Nova Sgr 1998 . Except for the line widths and continua shapes, the spectra have nearly the same emission lines.…”

Section: Reddening and Distancesupporting

confidence: 78%

“…Even though He i 1.0830 m was the strongest line in the spectrum in 2000 July, it only exceeded the Pa line flux by a factor of 3. A factor of a 10-20 is more common (Rossano et al 1994;Rudy et al 2002b;Venturini et al 2002).…”

Section: The Early Spectrummentioning

confidence: 99%

“…Although the age and speed class of the novae shown here vary, all are in the early to intermediate excitation stage. Venturini et al 2000;Rudy et al 2001), andV4633 Sgr (=Nova Sgr 1998;Lynch et al 2001). In Figure 10, we show all four spectra.…”

Section: Reddening and Distancementioning

confidence: 99%

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Time Development of Recurrent Nova CI Aquilae's 2000 Outburst between 0.8 and 2.5 MICRONS

Lynch¹,

Wilson²,

Rudy³

et al. 2004

Astron J

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We report 0.8-2.5 m spectrophotometry of CI Aquilae at eight epochs between 2000 May 9 and 2001 June 2 UT, corresponding to approximately 3 and 391 days after peak brightness. Near peak brightness, the spectra showed emission lines that were characteristic of a low-excitation, nitrogen-rich shell. Within a few weeks, the spectra began to show higher excitation/ionization emission lines indicative of a harder illuminating source: the neutral metal lines faded, leaving only lines of H i, He i, and He ii and the emerging coronal lines. A month after peak brightness, the [Ca viii] coronal line at 2.3205 m appeared and persisted until the last of our observations, on day +391. From the O i line ratios, we deduced a reddening of E BÀV = 1.5 AE 0.1 and a visual extinction of A V = 4.6 AE 0.2. Along with the rate of decline from the light curve (t 2 ), we derived a distance of 2.6 AE 1.3 kpc. The frequently observed unidentified novae lines were present in CI Aquilae along with a potentially new member of the group at 2.425 AE 0.002 m.

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Section: Reddening and Distancesupporting

confidence: 78%

Section: The Early Spectrummentioning

confidence: 99%

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Time Development of Recurrent Nova CI Aquilae's 2000 Outburst between 0.8 and 2.5 MICRONS

Lynch¹,

Wilson²,

Rudy³

et al. 2004

Astron J

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“…The excitation of the system was also sufficient to produce emission lines of He ii. Interestingly, some of the common coronal lines (e.g., [Ca viii Rudy et al (2002) and seen in several other novae (Williams, Longmore, & Geballe 1996;Lynch et al 2001;Venturini et al 2002) are present, but these appear to require only moderate excitation to exist. (Williams, Longmore, & Geballe [1996] identified the feature at 1.5545 lm with the hydrogenic 10-9 transition of N v, but Rudy et al [2002] rejected this identification based on the width of the feature, and the absence of the 9-8 multiplet and several other transitions from lower levels.)…”

Section: Late-time Spectrummentioning

confidence: 99%

Near‐Infrared Spectrophotometry and the CO Emission in V2274 Cygni (Nova Cygni 2001 No. 1)

Rudy

Dimpfl

Lynch

et al. 2003

ApJ

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Infrared spectroscopy of V2274 Cygni (=Nova Cygni 2001 No. 1) is presented for two widely separated epochs, 17 and 370 days after discovery. In addition to the Paschen and Brackett series of H i, the early-time spectrum shows strong emission lines of C i and N i, fluorescently excited lines of O i, and emission from the first overtone of carbon monoxide. Because the initial data were probably acquired no more than 18 days after outburst, CO molecule formation occurred remarkably quickly in the dense, cool, carbon and oxygen rich ejecta. Rapid formation was also seen in NQ Vul, V842 Cen, and V705 Cas, three other novae in which first-overtone CO emission has been detected. Formation of the CO molecule may occur chemically in a process that requires H 2 as a precursor or directly through radiative association. The overtone emission of V2274 Cyg indicates a temperature of $2500 K. The vibrational levels show no obvious departures from thermal equilibrium, which may indicate high optical depths in the fundamental. A large 13 C/ 12 C ratio (0:83 AE 0:3) is also indicated by the observations, consistent with the fast CNO burning expected in novae explosions. By the time of the second epoch observations, the emission lines of the neutral C, N, and O had disappeared. He i 10830 was the dominant emission feature in the spectrum. In addition to the hydrogen lines, recombination features of He ii were also strong. The common nebular lines of [S iii] were seen but only two coronal line, [S viii] 9911 and [Si vi] 19645, were detected. The CO emission had disappeared, but a strong thermal dust component was present. The interstellar reddening for the system was found to be E(BÀV Þ ¼ 1:3. This extinction, together with the absolute magnitude derived from the rate of decline of the light curve, suggest a distance of $10.8 kpc. This places V2274 Cyg well out of the Galactic plane. The small number of novae with spectroscopic detections of carbon monoxide all have prominent C i lines, moderate speed classes and ejection velocities, exhibit marked dust formation events, and result from an explosion on a CO-type white dwarf. Based on these similarities, the spectrum of V2274 is proposed as a likely near-infrared spectral template for other novae that display carbon monoxide emission.

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“…Depending on the evolution of the dust shells created in the outbursts, a variety of emission lines are seen in early post-outburst near-IR spectra. Moreover, for older novae the peak emission from the dust shells is shifted to longer wavelengths (e.g., Venturini et al 2002;. Four objects seen with the extreme colours in the plots of Our data taken during the quiescent phase (on April 2010) show the remnant of Nova Sgr 2001 as a relatively blue object, with the maximum intensity in the near-IR around the H-band (see Fig.…”

Section: Notesmentioning

confidence: 76%

A near-infrared catalogue of the Galactic novae in the VVV survey area

Saito

Minniti

Angeloni

et al. 2013

A&A

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Context. Near-infrared data on classical novae contain useful information about the ejected gas mass and the thermal emission by dust formed during eruption, and provide independent methods to classify the objects according to the colour of their progenitors, and the fading rate and features seen after eruption. The VISTA Variables in the Vía Láctea survey (VVV) is a near-IR ESO Public Survey mapping the Milky Way bulge and southern plane. Data taken during 2010-2011 covered the entire area in the JHK s bands plus some epochs in K s -band of the ongoing VVV variability campaign. Aims. We used the VVV data to create a near-IR catalogue of the known Galactic novae in the 562 sq. deg. area covered by VVV. We also compiled the information about novae from the variability tables of the VVV variability campaign. Methods. We used the novae list provided by VSX/AAVSO catalogue to search for all objects within the VVV area. From the 140 novae, we were able to retrieve the JHK s colours of 93 objects. We also checked in the ongoing VVV variability campaign for the light curves of novae that erupted in the last years. Results. The VVV near-IR catalogue of novae contains JHK s photometry of 93 objects completed as of December 2012. VVV allows to monitor objects within up to ΔK s ∼ 10 mag range. VVV images can also be used to discover and study novae by searching for the expanding shell. Since objects are seen at different distances and reddening levels, the colour-magnitude and colour-colour diagrams show the novae spread in magnitude as well as in colour. Dereddened colours and reddening-free indices were used with caution and cannot be a good approach in all cases since the distance and spectral features prevent more conclusive results for some extreme objects. Light curves for some recent novae are presented. Conclusions. Thanks to its high spatial resolution in the near IR and wide K s -range, the VVV survey can be a major contributor to the search for and study of novae in the most crowded and high-extinction regions of the Milky Way. The VVV survey area contains ∼35% of all known novae in the Galaxy.

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Near-Infrared Spectroscopy of Nova Sagittarius 1999 (V4444 Sagittarii)

Cited by 14 publications

References 26 publications

Time Development of Recurrent Nova CI Aquilae's 2000 Outburst between 0.8 and 2.5 MICRONS

Time Development of Recurrent Nova CI Aquilae's 2000 Outburst between 0.8 and 2.5 MICRONS

Near‐Infrared Spectrophotometry and the CO Emission in V2274 Cygni (Nova Cygni 2001 No. 1)

A near-infrared catalogue of the Galactic novae in the VVV survey area

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