Eta Carinae. II. The Spectrum.

Gaviola, E.

doi:10.1086/145746

Cited by 52 publications

(60 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For cycle 13, this zero point corresponds to HJD 2,456,865.2. The spectroscopic cycles are numbered since the first observed low/high state transition in 1948 (Gaviola 1953) as discovered by Damineli (1996), with the recent 2014 minimum corresponding to the beginning of cycle 13, leading to the ephemeris φ = (HJD − 2, 452, 819.2) 2022.7 + 11.…”

Section: Observationsmentioning

confidence: 99%

Tov_∞and beyond! The He i absorption variability across the 2014.6 periastron passage of η Carinae

Richardson

Madura

St-Jean

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Section: Observationsmentioning

confidence: 99%

Tov_∞and beyond! The He i absorption variability across the 2014.6 periastron passage of η Carinae

Richardson

Madura

St-Jean

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

“…These two sets of data cover the whole wavelength range of the VLT/X-shooter observations excluding gaps. Additionally, for some line identifications we used the data of Gaviola (1953), Johansson (1977), and Allen et al (1985).…”

Section: and Mesa-delgado Et Al (2009)mentioning

confidence: 99%

VLT/X-shooter observations of blue compact galaxies Haro 11 and ESO 338-IG 004

Гусева

Izotov

Fricke

et al. 2012

A&A

View full text Add to dashboard Cite

Context. Strongly star-forming galaxies of subsolar metallicities are typical of the high-redshift universe. Here we therefore provide accurate data for two low-z analogs, the well-known low-metallicity emission-line galaxies Haro 11 and ESO 338-IG 004. Aims. Our main goal is to derive their spectroscopic properties and to examine whether a previously reported near-infrared (NIR) excess in Haro 11 can be confirmed. Methods. On the basis of Very Large Telescope/X-shooter spectroscopic observations in the wavelength range ∼λλ3000-24 000 Å, we use standard direct methods to derive physical conditions and element abundances. Furthermore, we use X-shooter data together with Spitzer observations in the mid-infrared range to attempt to find hidden star formation. Results. We derive interstellar oxygen abundances of 12 + log O/H = 8.33 ± 0.01, 8.10 ± 0.04, and 7.89 ± 0.01 in the two H ii regions B and C of Haro 11 and in ESO 338-IG 004, respectively. The observed fluxes of the hydrogen lines correspond to the theoretical recombination values after correction for extinction with a single value of the extinction coefficient C(Hβ) across the entire wavelength range from the near-ultraviolet to the NIR and mid-infrared for each of the studied H ii regions. Thus, we confirm our previous findings obtained for several low-metallicity emission-line galaxies (Mrk 59, II Zw 40, Mrk 71, Mrk 996, SBS 0335-052E, PHL 293B, and GRB HG 031203) that the extinction coefficient C(Hβ) is not higher in the NIR than in the optical range and therefore that there are no emission-line regions contributing to the line emission in the NIR range, which are hidden in the optical range. The agreement between the extinction-corrected and CLOUDY-predicted fluxes implies that a H ii region model including only stellar photoionisation is able to account for the observed fluxes, in both the optical and NIR ranges. No additional excitation mechanism such as shocks from stellar winds and supernova remnants is needed. All observed spectral energy distributions (SEDs) can be reproduced quite well across the whole wavelength range by model SEDs except for Haro 11B, where there is a continuum flux excess at wavelengths >1.6 μm. It is possible that one or more red supergiant stars are responsible for the NIR flux excess in Haro 11B. We find evidence of a luminous blue variable (LBV) star in Haro 11C.

show abstract

“…The 5.52 year period proposed by Damineli (1996) was based on the epochs of the two bestobserved low excitation events of June 1992 and April 1948 (Gaviola, 1953) and indications of reoccurrence from the events of 1981. 49, 1987.04 and 1992.42.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Eta Carinae: a long period binary?

1997

View full text Add to dashboard Cite

We present new observations of 71 Carinae, strongly suggesting that it is a binary system. High dispersion measurements of the broad Pay emission line show periodic radial velocity variations that are nicely explained by a star in a highly eccentric orbit. Velocity characteristics of the system imply massive components, in accord with the luminosity and spectral characteristics. Strong and variable wind-wind interactions are predicted to take place in v Car on the basis of the orbital elements and physical characteristics of the components. The low excitation event predicted for the end of 1997 is underway, confirming the high coherence of the 5.52 year cycle and adding confidence to 77 Car as a binary system. We associate this event with periastron passage. A conclusive demonstration of the binary orbit is still pending, but the present work has the advantages of bringing this mysterious object within a stellar evolution framework, and, for the first time in its history, predictions suitable for testing against future observations. 0 1997 Elsevier Science B.V.

show abstract

Eta Carinae. II. The Spectrum.

Cited by 52 publications

References 0 publications

Tov_∞and beyond! The He i absorption variability across the 2014.6 periastron passage of η Carinae

Tov_∞and beyond! The He i absorption variability across the 2014.6 periastron passage of η Carinae

VLT/X-shooter observations of blue compact galaxies Haro 11 and ESO 338-IG 004

Eta Carinae: a long period binary?

Contact Info

Product

Resources

About

Eta Carinae. II. The Spectrum.

Cited by 52 publications

References 0 publications

Tov∞and beyond! The He i absorption variability across the 2014.6 periastron passage of η Carinae

Tov∞and beyond! The He i absorption variability across the 2014.6 periastron passage of η Carinae

VLT/X-shooter observations of blue compact galaxies Haro 11 and ESO 338-IG 004

Eta Carinae: a long period binary?

Contact Info

Product

Resources

About

Tov_∞and beyond! The He i absorption variability across the 2014.6 periastron passage of η Carinae

Tov_∞and beyond! The He i absorption variability across the 2014.6 periastron passage of η Carinae