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Luminosity-Metallicity Relation for Dirr Galaxies in the Near-Infrared

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Luminosity-Metallicity Relation for Dirr Galaxies in the Near-Infrared A&A 487, 901–920 (2008) Astronomy DOI: 10.1051/0004-6361:20077617 & c ESO 2008 Astrophysics Luminosity-metallicity relation for dIrr galaxies in the near-infrared I. Saviane1,V.D.Ivanov1,E.V.Held2, D. Alloin3,R.M.Rich4, F. Bresolin5, and L. Rizzi6 1 European Southern Observatory, Alonso de Cordova, 3107 Santiago, Chile e-mail: [isaviane;vivanov]@eso.org 2 OAPD, vicolo Osservatorio 5, 35122 Padova, Italy e-mail: [email protected] 3 AIM, CEA/DSM/IRFU-Université Paris 7, Service d’Astrophysique, CEA/Saclay, 91191 Gif-sur-Yvette Cedex, France e-mail: [email protected] 4 Department of Physics and Astronomy, 430 Portola Plaza, UCLA, Los Angeles, CA 90095-1547, USA e-mail: [email protected] 5 Institute for Astronomy, University of Hawaii at Manoa, 2680 Woodlawn Drive, Honolulu, HI 96822, USA e-mail: [email protected] 6 Joint Astronomy Centre, 660 N. A’ohoku Place, University Park, Hilo, HI 96720, USA e-mail: [email protected] Received 5 April 2007 / Accepted 22 May 2008 ABSTRACT Context. The luminosity-metallicity relation is one of the fundamental constraints in the study of galaxy evolution; yet none of the relations available today has been universally accepted by the community. Aims. The present work is a first step to collect homogeneous abundances and near-infrared (NIR) luminosities for a sample of dwarf irregular (dIrr) galaxies, located in nearby groups. The use of NIR luminosities is intended to provide a better proxy to mass than the blue luminosities commonly used in the literature; in addition, selecting group members reduces the impact of uncertain distances. Accurate abundances are derived to assess the galaxy metallicity. Methods. Optical spectra are collected for H ii regions in the dIrrs, allowing the determination of oxygen abundances by means of the temperature-sensitive method. For each dIrr galaxy H-band imaging is performed and the total magnitudes are measured via surface photometry. Results. This high-quality database allows us to build a well-defined luminosity-metallicity relation in the range −13 ≥ MH ≥ −20. The scatter around its linear fit is reduced to 0.11 dex, the lowest of all relations currently available. There might exist a difference between the relation for dIrrs and the relation for giant galaxies, although a firm conclusion should await direct abundance determinations for a significant sample of massive galaxies. Conclusions. This new dataset provides an improved luminosity-metallicity relation, based on a standard NIR band, for dwarf star- forming galaxies. The relation can now be compared with some confidence to the predictions of models of galaxy evolution. Exciting follow-ups of this work are (a) exploring groups with higher densities, (b) exploring nearby galaxy clusters to probe environmental effects on the luminosity-metallicity relation, and (c) deriving direct oxygen abundances in the central regions of star-forming giant galaxies, to settle the question of a possible dichotomy between the chemical evolution of dwarfs and that of massive galaxies. Key words. galaxies: fundamental parameters – infrared: galaxies – galaxies: dwarf – galaxies: irregular – galaxies: ISM 1. Introduction observed in spheroidal galaxies (e.g. Caldwell et al. 1992), mostly field galaxies, in which old stellar populations dominate, According to standard scenarios of galactic chemical evolution, and for which the chemical evolution has stopped. Do we ex- − a luminosity-metallicity (L Z) relation is established through pect a similar behaviour in the case of dwarf irregular galaxies galactic winds – induced by supernova explosions – removing (dIrr)? The situation is more complex. First, dIrrs are still active the interstellar medium (ISM) before it has been totally con- (in the sense of star formation), exhibiting substantial gas frac- verted into stars (see the seminal work of Larson 1974;andalso tions and a broad range of star-formation rates (SFR). So, one Tinsley & Larson 1979; Dekel & Silk 1986; Lynden-Bell 1992, would expect to encounter in Irrs, ISMs of different chemical ffi among others). As this process is more e cient in low-mass maturities and rapidly evolving luminosities: all factors which (low escape velocity) galaxies, less metals should be trapped would loosen any established relation between mass and metal- − in dwarf galaxies. Indeed, a well-defined L Z relation is licity. Second, the available sample of dIrrs is made of galaxies belonging to groups rather than distributed in the field. It is well Based on data collected at the European Southern Observatory, known that the evolution of a galaxy gas content depends on its La Silla, Chile, Proposal N. 70.B-0424(A,B); based on observations environment, and that gas stripping is boosted through galaxy made at Lick (UCO) Observatory; based on observations made with interactions in dense groups and cluster sub-clumps. So, while the William Herschel Telescope operated on the island of La Palma by one can see reasons why the terminal chemical evolution in dIrrs the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. might depend on the galactic mass – similarly to the sample of Article published by EDP Sciences 902 I. Saviane et al.: L − Z relation of dIrr galaxies gas-free spheroidal galaxies, there are a number of extra pro- galaxy orders of magnitudes more massive but lacking a recent cesses blurring the situation. Hence, it is unclear whether star formation episode. In comparison, a recent starburst is at dIrr galaxies should exhibit a luminosity-metallicity relation. most 10 times brighter in the near-infrared (NIR) than its under- Under such a scenario dwarf galaxies lose substantial frac- lying old population of same mass. Therefore, the NIR window tions of their mass in the course of their evolution, and should be being more stable with regard to star formation episodes is more major contributors to the chemical evolution of the inter-galactic appropriate for probing the galaxy basic properties, such as its medium (IGM). In particular, mass loss through galactic winds mass. should occur in dIrr galaxies: their study contributes to probe the In order to address these issues, we embarked on a medium- fraction of the IGM enrichment which is due to dwarf galaxies term project aimed at gathering nebular oxygen abundances and in general (e.g., Garnett 2002). Losses of enriched gas in dwarf NIR luminosities for a sample of dIrrs belonging to the three galaxies have indeed been observed: Martin et al. (2002)de- nearest groups of galaxies. In this way we can test the exis- 6 tected a galactic wind of ∼6 × 10 M from NGC 1569, and tence of an L − Z relation in well-defined environments (char- for the first time, they could measure its metallicity. The authors acterized by the group density), for which the scatter in apparent 4 concluded at 3 × 10 M of oxygen in the wind, almost as much distance modulus is low, and for which an homogeneous set of as in the disk of the dwarf itself. Hence, the cosmic chemical abundances can be obtained. evolution and the existence of an L − Z relation appear to be Since we started the project, a few investigations have been closely inter-related: this was an additional motivation to pursue published, in relation with the context presented above. The the study presented here. first L − Z relation using NIR luminosities (aside the work by The case of another dIrr, SagDIG, further illustrates this Saviane et al. 2004) is that by Salzer et al. (2005, hereafter S05). point. In one of our previous studies (Saviane et al. 2002)we Their sample is dominated by massive galaxies, and their rela- measured a very low oxygen content (7.26 ≤ 12 + log (O/H) ≤ tion was derived using 2MASS data for the luminosities, and 7.50), a result which is not compatible with a closed-box evo- proprietary spectra from the KPNO International Spectroscopic lution. According to the model, such a low abundance would Survey (KISS) for the metallicities. The 2MASS survey having a imply a large gas mass fraction μ = mgas/(mgas + mstars) ≈ 0.97, relatively shallow limiting magnitude, for a few additional dwarf whereas the observed gas mass fraction is only μ ≈ 0.86. It is galaxies NIR photometry was supplemented by the authors. At 6 easy to compute that ≈1.5 × 10 M of gas are missing, and, the other extreme, the sample assembled by Mendes de Oliveira since this mass is smaller than that of the NGC 1569 galactic et al. (2006) is entirely made of dwarf galaxies. They gathered wind, it is plausible to conclude that SagDIG lost some of its gas K-band luminosities and metallicities – obtained through the di- into the IGM. rect method – for 29 dIrrs. The NIR data are from 2MASS or On the other hand, a cautionary remark should be added, from Vaduvescu et al. (2005), and metallicities have been picked since a general consensus on the role of galactic winds in up from a variety of sources. Finally Lee et al. (2006)haveused the evolution of dwarf galaxies and the IGM has not been the Spitzer Infrared Array Camera to compute 4.5 μm luminosi- reached yet. For example, by means of chemo-photometric mod- ties for ∼30 nearby dIrrs, the distance of which have been de- els Calura & Matteucci (2006) conclude that dIrr galaxies play rived using standard candles. With oxygen abundances collected a negligible role in the enrichment of the IGM, and the numeri- from the literature, they constructed a 4.5 μm L − Z relation. cal models of Silich & Tenorio-Tagle (1998) show that galactic Although these studies have certainly improved the situation, winds never reach the escape velocity of these dwarfs.
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