Spectroscopic Properties and Luminosity Distribution of the Universidad Complutense de Madrid Survey Galaxies

Gallego, J.; Zamorano, J.; Rego, M.; Vitores, A. G.

doi:10.1086/303551

Cited by 74 publications

(99 citation statements)

References 32 publications

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“…Given that the luminosity function is well fitted as a Schechter function, and , a ≤ Ϫ2 can be integrated for the whole range of luminosities: 10 for a total of 1 dex. This luminosity density is similar to the one we could estimate from the B-band luminosity function published by Gallego et al (1997) for the UCM sample. It is also comparable to the luminosity density we would obtain if we apply an average [O ii] l3727/Ha factor to the extinction-corrected Ha luminosity density measured by Gallego et al (1995).…”

Section: The Evolution Of the [O Ii] L3727 Luminosity Densitysupporting

confidence: 88%

The [OII]λ3727 Luminosity Function of the Local Universe

Maestro

Dabó

Calvo

et al. 2003

Highlights of Spanish Astrophysics III

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The measurement of the star formation rate density of the universe is of prime importance in understanding the formation and evolution of galaxies. The [O ii] l3727 emission-line flux, easy to measure up to z ≈ 1.4 within deep redshift surveys in the optical and up to in the near-infrared, offers a reliable means of z ≈ 5.4 characterizing the star formation properties of high-z objects. In order to provide the high-z studies with a local reference, we have measured total [O ii] l3727 fluxes for the well-analyzed local sample of star-forming galaxies from the Universidad Complutense de Madrid Survey. These data are used to derive the [O ii] l3727 luminosity function for local star-forming galaxies. When compared with similar luminosity densities published for redshift up to , the overall evolution already observed in the star formation activity of the universe is confirmed. z ≈ 1

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Section: The Evolution Of the [O Ii] L3727 Luminosity Densitysupporting

confidence: 88%

The [OII]λ3727 Luminosity Function of the Local Universe

Maestro

Dabó

Calvo

et al. 2003

Highlights of Spanish Astrophysics III

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“…6: Rönnback and Bergvall (1995). 7: Gallego et al (1997). 8: Vitores et al (1996), assuming B − R = 0.6.…”

Section: Discussionmentioning

confidence: 99%

“…The reason is that the Case survey also is sensitive to galaxies with a low level of HII activity. A comparison of derived space densities of emission line/UV-excess dwarfs is given by and Gallego et al (1997). These differences demonstrate once more that different surveys effectively target different types of galaxies.…”

Section: Luminosity Functionmentioning

confidence: 99%

“…The higher the dispersion, the easier it becomes to detect weak emission lines against the continuum, while a narrow spectral range cuts significantly the sky background at the expense of the redshift range. The recent surveys discussed in Gallego et al (1997) and Salzer (1999) use the Hα line which can be bright even in low-excitation or very metal-poor objects. Because each technique involves specific observational biases, modern surveys tend to combine various approaches.…”

Section: Ground-based Selectionmentioning

confidence: 99%

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The most metal-poor galaxies

Kunth

Östlin

2000

Astronomy and Astrophysics Review

381

428

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Metallicity is a key parameter that controls many aspects in the formation and evolution of stars and galaxies. In this review we focus on the metal deficient galaxies, in particular the most metal-poor ones, because they play a crucial rôle in the cosmic scenery. We first set the stage by discussing the difficult problem of defining a global metallicity and how this quantity can be measured for a given galaxy. The mechanisms that control the metallicity in a galaxy are reviewed in detail and involve many aspects of modern astrophysics: galaxy formation and evolution, massive star formation, stellar winds, chemical yields, outflows and inflows etc. Because metallicity roughly scales as the galactic mass, it is among the dwarfs that the most metalpoor galaxies are found. The core of our paper reviews the considerable progress made in our understanding of the properties and the physical processes that are at work in these objects. The question on how they are related and may evolve from one class of objects to another is discussed. While discussing metal-poor galaxies in general, we present a more detailed discussion of a few very metal-poor blue compact dwarf galaxies like IZw18. Although most of what is known relates to our local universe, we show that it pertains to our quest for primeval galaxies and is connected to the question of the origin of structure in the universe. We discuss what QSO absorption lines and known distant galaxies tell us already? We illustrate the importance of star-forming metal-poor galaxies for the determination of the primordial helium abundance, their use as distance indicator and discuss the possibility to detect nearly metal-free galaxies at high redshift from Lyα emission.

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“…6.-Excitation as a function of rest-frame absolute blue magnitude for the galaxies in our sample (large symbols, labeled as in Fig. 5), compared to the sample of nearby UCM (z < 0:045) emission-line galaxies of Gallego et al (1996Gallego et al ( , 1997 (small symbols). The rest-frame absolute B magnitudes for the VCM sample have been extracted from the data presented by Pérez-González et al (2002) and were corrected for Galactic extinction using the dust maps of Schlegel et al (1998).…”

Section: Sfr From Ultraviolet Continuamentioning

confidence: 96%

A Multiwavelength Approach to the Star Formation Rate Estimation in Galaxies at Intermediate Redshifts

Cardiel

Elbaz

Schiavon

et al. 2003

ApJ

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We use a sample of seven starburst galaxies at intermediate redshifts (z $ 0:4 and 0.8) with observations ranging from the observed ultraviolet to 1.4 GHz, to compare the star formation rate (SFR) estimators that are used in the different wavelength regimes. We find that extinction-corrected H underestimates the SFR, and the degree of this underestimation increases with the infrared luminosity of the galaxies. Galaxies with very different levels of dust extinction as measured with SFR IR /SFR(H , uncorrected for extinction) present a similar attenuation A[H ], as if the Balmer lines probed a different region of the galaxy than the one responsible for the bulk of the IR luminosity for large SFRs. In addition, SFR estimates derived from [O ii] 3727 match very well those inferred from H after applying the metallicity correction derived from local galaxies. SFRs estimated from the UV luminosities show a dichotomic behavior, similar to that previously reported by other authors in galaxies at zd0:4. Here we extend this result up to z $ 0:8. Finally, one of the studied objects is a luminous compact galaxy (LCG) that may be suffering similar dust-enshrouded star formation episodes. These results highlight the relevance of quantifying the actual L IR of LCGs, as well as that of a much larger and generic sample of luminous infrared galaxies, which will be possible after the launch of SIRTF.

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Spectroscopic Properties and Luminosity Distribution of the Universidad Complutense de Madrid Survey Galaxies

Cited by 74 publications

References 32 publications

The [OII]λ3727 Luminosity Function of the Local Universe

The [OII]λ3727 Luminosity Function of the Local Universe

The most metal-poor galaxies

A Multiwavelength Approach to the Star Formation Rate Estimation in Galaxies at Intermediate Redshifts

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