Evolutionary Synthesis Modeling of Red Supergiant Features in the Near‐Infrared

Origlia, L.; Goldader, J. D.; Leitherer, Claus; Schaerer, D.; Oliva, E.

doi:10.1086/306937

Cited by 58 publications

(81 citation statements)

References 45 publications

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“…8) resemble, in part, the spectra of NGC 4941 (Seyfert 2) and NGC 4579 (LINER), superposed on a normal galaxy spectrum, such as NGC 3368 (see references quoted in NED for these galaxies). The absorption features in the spectrum of HRG 54103 (in the λλ 5800−7200 Å region) suggest the contribution of intermediate-mass stars (see Origlia et al 1999;Guzeva et al 2000;Fernandes et al 2004). The spectra of the ring sections exhibit star forming characteristics.…”

Section: Spectramentioning

confidence: 95%

The ring galaxy HRG 54 103: a first study

Faúndez-Abans

Fernandes

Oliveira-Abans

et al. 2009

A&A

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Aims. We report the first study of the peculiar ring galaxy HRG 54103 which was previously classified as a Saturn-like type galaxy. Methods. The study is based on low resolution spectroscopy and photometric observations in the optical band to highlight the characteristics of this almost isolated galaxy. The colour distribution of HRG 54103 was examined through direct CCD BVRI Kron-Cousins system imagery. Color-color diagrams of the bulge and ring are displayed and further compared with the star-forming ring galaxy HRG 2302.Results. The results of image enhancement of the morphological structure of this galaxy are discussed. The nuclear emission-line spectrum resembles that of a Seyfert2/LINER object, with z = 0.022 and heliocentric V = 6483 ± 18 km s −1 , in agreement with the literature. The nuclear, bulge and ring section radial velocities along the ring major axis show a peculiar distribution, which together and the disk-ring asymmetry suggest a possible merger event in the recent past of this object, which could also have caused its formation.

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Section: Spectramentioning

confidence: 95%

The ring galaxy HRG 54 103: a first study

Faúndez-Abans

Fernandes

Oliveira-Abans

et al. 2009

A&A

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“…Both observations and evolutionary models (see, e.g., Keller 1999;Origlia et al 1999;Origlia 2003 and references therein) suggest that RSGs of ages between $6 and 100 Myr and metallicities between 1/10 solar and solar are characterized by low gravities (log g < 1:0), low temperatures ( 4000 K), and relatively high microturbulence velocity ( ! 3 km s À1 ).…”

Section: Ir Spectra and Stellar Abundancesmentioning

confidence: 99%

Stellar and Gaseous Abundances in M82

Origlia

Ranalli

Comastri

et al. 2004

ApJ

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The near-infrared (near-IR) absorption spectra of starburst galaxies show several atomic and molecular lines from red supergiants that can be used to infer reliable stellar abundances. The metals locked in stars give a picture of the galaxy metallicity prior to the last burst of star formation. The enrichment of the new generation of stars born in the last burst can be traced by measuring the hot gas in the X-rays. For the first time, detailed stellar abundances in the nuclear region of the starburst galaxy M82 have been obtained. They are compared with those of the hot gas, as derived from an accurate reanalysis of the XMM-Newton and Chandra nuclear X-ray spectra. The cool stars and the hot gas suggest Fe=H ½ ¼À0:35 AE 0:2 dex and an overall [Si / Fe] and [Mg / Fe] enhancement by $0.4 and 0.5 dex, respectively. This is consistent with a major chemical enrichment by Type II supernova explosions in recursive bursts on short timescales. Oxygen is more puzzling to interpret, since it is enhanced by $0.3 dex in stars and depleted by $0.2 dex in the hot gas. None of the standard enrichment scenarios can fully explain such a behavior compared with that of the other -elements.

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“…Allowing for the well-known uncertainty in redsupergiant stellar evolutionary tracks (Langer & Maeder 1995;Mayya 1997;Origlia et al 1998;Leitherer et al 1999), especially at metallicities less than solar, it seems possible that the [255−555] color may be ∼0.2 mag too red. With all these possible factors, we prefer the explanation of a 9-13 Myr cluster with little to no extinction.…”

Section: Other F255w Sources: "Clump F" and The Central Cluster Of CLmentioning

confidence: 99%

The star cluster system of the NGC 7673 starburst

Homeier

Gallagher

Pasquali³

2002

A&A

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Abstract. We investigate the star cluster system in the starburst galaxy NGC 7673 using archival Hubble Space Telescope WFPC2 broad-band images. For the first time we are able to examine the internal structures of the prominent optical clumps in this galaxy. The clumps are composed of young stars, 16-33% of which are in bright star clusters. We identify 268 star cluster candidates in both the F555W and F814W images, and 50 clusters with the F255W filter. These data allow us to estimate ages and masses using color-magnitude and two-color diagrams for our sample. We find a population of young, <6 Myr clusters located throughout the galaxy with concentrations in the clumps. Star cluster mass estimates are 5-50 × 10 4 M for the brightest objects. The starburst remains active in physically well-separated regions, indicating a widespread starburst trigger. We discuss clump lifetimes, their implications for the future evolution of NGC 7673, and possible relationships to high redshift starbursts.

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Evolutionary Synthesis Modeling of Red Supergiant Features in the Near‐Infrared

Cited by 58 publications

References 45 publications

The ring galaxy HRG 54 103: a first study

The ring galaxy HRG 54 103: a first study

Stellar and Gaseous Abundances in M82

The star cluster system of the NGC 7673 starburst

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