On emission-line spectra obtained from evolutionary synthesis models

Villaverde, M.; Cerviño, M.; Luridiana, V.

doi:10.1051/0004-6361/200912549

Cited by 10 publications

(16 citation statements)

References 65 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Based on a first approximation, taking into account the models presented in Villaverde et al (2010), those high equivalentwidth galaxies in [O iii] λ5007 may be an analogous to our detected emitters with high [O ii]3727 equivalent width.…”

Section: [O Ii]3727 Equivalent Widthmentioning

confidence: 68%

“…They found that those galaxies can be classified as: low-mass, strong starbust, and compact. Following the models of Villaverde et al (2010), we can assume a maximum equivalent width of the [O ii]3727 line for 'normal' galaxies at 150 Å. Indeed, Kong et al (2002) found that galaxies with EW[O ii]3727>100 Å are in the 90th percentile and Thomas et al (2013), based on data from the SDSS-III/BOSS, showed that galaxies with EW[O ii]3727>100 Å are located outside the limits of their figures.…”

Section: [O Ii]3727 Equivalent Widthmentioning

confidence: 99%

See 1 more Smart Citation

The OTELO survey

Cedrés

Bongiovanni

Cerviño

et al. 2021

A&A

Self Cite

View full text Add to dashboard Cite

Aims. In this paper, we aim to study the main properties and luminosity function (LF) of the [O II]3727 emitters detected in the OTELO survey in order to characterise the star formation processes in low-mass galaxies at z ∼ 1.43 and to constrain the faint-end of the LF. Methods. Here, we describe the selection method and analysis of the emitters obtained from narrow-band scanning techniques. In addition, we present several relevant properties of the emitters and discuss the selection biases and uncertainties in the determination of the LF and the star formation rate density (SFRD). Results. We confirmed a total of 60 sources from a preliminary list of 332 candidates as [O II]3727 emitters. Approximately 93% of the emitters have masses in the range of 108 < M*/M⊙ < 109. All of our emitters are classified as late-type galaxies, with a lower value of (u − v) when compared with the rest of the emitters of the OTELO survey. We find that the cosmic variance strongly affects the normalisation (ϕ*) of the LF and explains the discrepancy of our results when compared with those obtained from surveys of much larger volumes. However, we are able to determine the faint-end slope of the LF, namely, α = −1.42 ± 0.06, by sampling the LF down to ∼1 dex lower than in previous works. We present our calculation of the SFRD of our sample and compare it to the value obtained in previous studies from the literature.

show abstract

Section: [O Ii]3727 Equivalent Widthmentioning

confidence: 68%

Section: [O Ii]3727 Equivalent Widthmentioning

confidence: 99%

The OTELO survey

Cedrés

Bongiovanni

Cerviño

et al. 2021

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…An extra caveat arises for clusters with stellar masses of < ∼ 10 4 M since in this regime the Initial Mass Function is not properly sampled and stochastic effects are important (e.g. Villaverde et al 2010).…”

Section: On the Relationship Between Extra N And Wr Starsmentioning

confidence: 99%

The ionized gas in the central region of NGC 5253

Monreal-Ibero

Walsh

Vı́lchez

2012

A&A

View full text Add to dashboard Cite

Context. Blue compact dwarf (BCD) galaxies constitute the ideal laboratories to test the interplay between massive star formation and the surrounding gas. As one of the nearest BCD galaxies, NGC 5253 was previously studied with the aim to elucidate in detail the starburst interaction processes. Some open issues regarding the properties of its ionized gas still remain to be addressed. Aims. The 2D structure of the main physical and chemical properties of the ionized gas in the core of NGC 5253 has been studied. Methods. Optical integral field spectroscopy (IFS) data has been obtained with FLAMES Argus and lower resolution gratings of the Giraffe spectrograph. Results. We derived 2D maps for different tracers of electron density (n e ), electron temperature (T e ) and ionization degree.

show abstract

“…Given that the continuum shape and luminosity control the emission line intensity in a non-linear way (see Villaverde et al 2010, for more details), using an average ionizing continuum of clusters in function of the cluster mass as input of photoionization codes, as synthesis models provide, gives unrealistic results.…”

Section: Effects In H II Regionsmentioning

confidence: 99%

Modeling the ionizing spectra of H II regions: individual stars versus stellar ensembles

Villaverde

Cerviño

Luridiana

2010

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We study how IMF sampling affects the ionizing flux and emission line spectra of low mass stellar clusters. Methods. We performed 2 × 10 6 Monte Carlo simulations of zero-age solar-metallicity stellar clusters covering the 20−10 6 M mass range. We study the distribution of cluster stellar masses, M clus , ionizing fluxes, Q(H 0 ), and effective temperatures, T clus eff . We compute photoionization models that broadly describe the results of the simulations and compare them with photoionization grids.Results. Our main results are: (a) a large number of low mass clusters (80% for M clus = 100 M ) are unable to form an H ii region. (b) There are a few overluminous stellar clusters that form H ii regions. These overluminous clusters preserve statistically the mean value of Q(H 0 ) obtained by synthesis models, but the mean value cannot be used as a description of particular clusters. (c) The ionizing continuum of clusters with M clus < ∼ 10 4 M is more accurately described by an individual star with self-consistent effective temperature (T * eff ) and Q(H 0 ) than by the ensemble of stars (or a cluster T clus eff ) produced by synthesis models. (d) Photoionization grids of stellar clusters cannot be used to derive the global properties of low mass clusters. Conclusions. Although variations in the upper mass limit, m up , of the IMF would reproduce the effects of IMF sampling, we find that an ad hoc law that relates m up to M clus in the modeling of stellar clusters is useless, since: (a) it does not cover the whole range of possible cases; and (b) the modeling of stellar clusters with an IMF is motivated by the need to derive the global properties of the cluster: however, in clusters affected by sampling effects we have no access to global information of the cluster but only particular information about a few individual stars.

show abstract

On emission-line spectra obtained from evolutionary synthesis models

Cited by 10 publications

References 65 publications

The OTELO survey

The OTELO survey

The ionized gas in the central region of NGC 5253

Modeling the ionizing spectra of H II regions: individual stars versus stellar ensembles

Contact Info

Product

Resources

About