Spectroscopic Observations of Seven Suspected Symbiotic Stars

Pereira, C. B.; Landaberry, S. J. C.; Conceição, F. da

doi:10.1086/300564

Cited by 12 publications

(13 citation statements)

References 20 publications

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“…Values around log(Ne)∼4 are found only in a few of the 146 planetary nebulae analysed by Stanghellini & Kaler (1989). Similar and higher densities are found in symbiotic stars (Pereira et al 1998;Schmid & Schild 1990;Gutiérrez-Moreno & Moreno 1996) and in young planetary nebulae like Hen 2-57 (Kingsburgh & Barlow 1994), Hen 2-35 (Corradi 1995), IC 4997 (Hyung, Aller & Feibelman 1994) and K 4-47 (Gonçalves et al 2004).…”

Section: Electron Densities Temperatures and Chemical Abundancesmentioning

confidence: 54%

Deep spectroscopy of the emission-line populations in NGC 185★

Gonçalves¹,

Magrini²,

Martins³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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Because dwarf galaxies are the most abundant type of galaxy, they are crucial for our understanding of the formation and evolution of galaxies. Abundance ratios and their variations as a result of star formation are key constraints in chemical evolution models. Thus, the determination of these abundances in the dwarf galaxies of the Local Universe is extremely important. However, these objects are intrinsically faint, and observational constraints to their evolution can be obtained only for very nearby galaxies. NGC 185 is one of the four brightest dwarf companions of M31. However, unlike the other three -NGC 147, 205 and 221 (M32) -it has an important content of gas and dust. We have obtained deep spectroscopic observations of the Hα emitting population of NGC 185 using the Gemini multi-object spectrograph at the Gemini North telescope. As a result, in addition to the bright planetary nebulae (PNe) previously found in the galaxy and reported in the literature, we have found other, much fainter, PNe. We have then recalculated the electron temperatures and chemical abundances of the brightest PNe and, for the first time, we have derived their electron densities. Our characterization of the population properties of the PNe is interpreted in terms of the chemical evolution of NGC 185, which suggests that it has suffered a significant chemical enrichment within the last ∼8 Gyr. We have also discovered the first symbiotic star in the galaxy and we have determined the properties of a known supernova remnant located close to the centre of NGC 185.

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Section: Electron Densities Temperatures and Chemical Abundancesmentioning

confidence: 54%

Deep spectroscopy of the emission-line populations in NGC 185★

Gonçalves¹,

Magrini²,

Martins³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…139=V2905 Sgr IRAS data from [92]. Spectral type of cool component also estimated in [245] to be K/M. 146=V3811 Sgr Mis-identified in [248] and in [19] (see [20]).…”

Section: =H 2−38mentioning

confidence: 94%

A catalogue of symbiotic stars

Belczyński

Mikołajewska

Munari

et al. 2000

Astron. Astrophys. Suppl. Ser.

379

407

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Abstract. We present a new catalogue of symbiotic stars. In our list we include 188 symbiotic stars as well as 30 objects suspected of being symbiotic. For each star, we present basic observational material: coordinates, V and K magnitudes, ultraviolet (UV), infrared (IR), X-ray and radio observations. We also list the spectral type of the cool component, the maximum ionization potential observed, references to finding charts, spectra, classifications and recent papers discussing the physical parameters and nature of each object. Moreover, we present the orbital photometric ephemerides and orbital elements of known symbiotic binaries, pulsational periods for symbiotic Miras, Hipparcos parallaxes and information about outbursts and flickering.

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“…Its optical spectrum shows a latetype continuum with prominent TiO bands and emission lines from the Balmer series, He I, [Ne III], [O III], and [FeVII]. The optical spectrum of Hen 3-461 resembles the spectrum of RT Cru and T CrB in quiescence (Pereira et al 1998), with a strong red continuum and weak Balmer lines. Little is known about this source at other wavelengths.…”

Section: Hen 3-461mentioning

confidence: 97%

Symbiotic stars in X-rays

Luna

Sokoloski

Mukai

et al. 2013

A&A

119

175

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Until recently, symbiotic binary systems in which a white dwarf accretes from a red giant were thought to be mainly a soft X-ray population. Here we describe the detection with the X-ray Telescope (XRT) on the Swift satellite of nine white dwarf symbiotics that were not previously known to be X-ray sources and one that had previously been detected as a supersoft X-ray source. The nine new X-ray detections were the result of a survey of 41 symbiotic stars, and they increase the number of symbiotic stars known to be X-ray sources by approximately 30%. The Swift/XRT telescope detected all of the new X-ray sources at energies greater than 2 keV. Their X-ray spectra are consistent with thermal emission and fall naturally into three distinct groups. The first group contains those sources with a single, highly absorbed hard component that we identify as probably coming from an accretion-disk boundary layer. The second group is composed of those sources with a single, soft X-ray spectral component that probably originates in a region where low-velocity shocks produce X-ray emission, i.e., a colliding-wind region. The third group consists of those sources with both hard and soft X-ray spectral components. We also find that unlike in the optical, where rapid, stochastic brightness variations from the accretion disk typically are not seen, detectable UV flickering is a common property of symbiotic stars. Supporting our physical interpretation of the two X-ray spectral components, simultaneous Swift UV photometry shows that symbiotic stars with harder X-ray emission tend to have stronger UV flickering, which is usually associated with accretion through a disk. To place these new observations in the context of previous work on X-ray emission from symbiotic stars, we modified and extended the α/β/γ classification scheme for symbiotic-star X-ray spectra that was introduced by Muerset et al. based upon observations with the ROSAT satellite, to include a new δ classification for sources with hard X-ray emission from the innermost accretion region. Because we have identified the elusive accretion component in the emission from a sample of symbiotic stars, our results have implications for the understanding of wind-fed mass transfer in wide binaries, and the accretion rate in one class of candidate progenitors of type Ia supernovae.

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Spectroscopic Observations of Seven Suspected Symbiotic Stars

Cited by 12 publications

References 20 publications

Deep spectroscopy of the emission-line populations in NGC 185★

Deep spectroscopy of the emission-line populations in NGC 185★

A catalogue of symbiotic stars

Symbiotic stars in X-rays

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