Violent star formation in NGC 2363

Gonzalez-Delgado, R. M.; Pérez, E.; Tenorio-Tagle, G.; Vı́lchez, J. M.; Terlevich, Elena; Terlevich, R.; Telles, E.; Rodríguez-Espinosa, J. M.; Mas-Hesse, J. M.; García-Vargas, María Luisa; Díaz, Ángeles I.; Cepa, J.; Castañeda, H. O.

doi:10.1086/174992

Cited by 134 publications

(163 citation statements)

References 0 publications

Supporting

Mentioning

147

Contrasting

Order By: Relevance

“…Using the current data set, DUCBR showed that the intensity of the weak broad component in Hα is 2-3% that of the narrow component, in agreement with the results of Gonzalez-Delgado et al (1994).…”

Section: The Observationssupporting

confidence: 85%

“…In NGC 2363, this broad component, first reported by Roy et al (1992), appears as a faint pedestal under the narrow Hα, Hβ and [O iii] lines of the socalled knot A (Gonzalez-Delgado et al 1994). This pedestal has an fwhm in excess of 2300 km s −1 (Drissen et al 2009, hereafter DUCBR).…”

Section: Introductionmentioning

confidence: 92%

“…It suggests that the physical conditions pertaining to the gas that produces the faint broad wings are very likely similar to those of the more quiescent nebular gas. 6 The amount of dust encountered by Gonzalez-Delgado et al (1994) for the narrow line emitting gas in knot A is as little as C(Hβ) = 0.2 (or τ V = 0.22). Uncertainties in our absolute calibration of the blue spectrum does not allow us to verify this value.…”

Section: Characteristics Of the Broad Profile Wingsmentioning

confidence: 99%

See 2 more Smart Citations

The broad Hα, [O III] line wings in stellar supercluster A of NGC 2363 and the turbulent mixing layer hypothesis

Binette

Drissen

Úbeda

et al. 2009

A&A

View full text Add to dashboard Cite

Context. Supercluster A in the extragalactic H ii region NGC 2363 is remarkable for the hypersonic gas seen as faint extended broad emission lines with a full-width zero intensity of 7000 km s −1 . Aims. We explore the possibility that the observed broad profiles are the result of the interaction of a high-velocity cluster wind with dense photoionized clumps. Methods. The geometry considered is that of near static photoionized condensations at the surface of which turbulent mixing layers arise as a result of the interaction with the hot wind. The approximative treatment of turbulence was carried out using the mixing length approach of Cantó & Raga. The code mappings ic was used to derive the mean quantities describing the flow and to compute the line emissivities within the turbulent layers. The velocity projection in three dimensions of the line sources was carried out analytically. is uncomfortably high and alternative processes that would provide comparable constant acceleration of the emission gas up to 4000 km s −1 might have to be considered.

show abstract

Section: The Observationssupporting

confidence: 85%

Section: Introductionmentioning

confidence: 92%

Section: Characteristics Of the Broad Profile Wingsmentioning

confidence: 99%

See 1 more Smart Citation

The broad Hα, [O III] line wings in stellar supercluster A of NGC 2363 and the turbulent mixing layer hypothesis

Binette

Drissen

Úbeda

et al. 2009

A&A

View full text Add to dashboard Cite

show abstract

“…According to the models computed by González-Delgado et al (1994), for the helium abundance derived for the region 74C (see next section), this ∆ Pa/I(Hβ) implies an electron temperature of 8000 ± 700 K, which agrees with that derived from the [SIII] lines within the errors. Therefore, no temperature fluctuations are apparent in the region which (Pérez 1997).…”

Section: Physical Conditions Of the Gassupporting

confidence: 78%

Chemical abundances and ionizing clusters of H ii regions in the LINER galaxy NGC 4258

Díaz¹,

Castellanos²,

Terlevich³

et al. 2000

Monthly Notices RAS

Self Cite

View full text Add to dashboard Cite

We present long-slit observations in the optical and near infrared of eight H II regions in the spiral galaxy NGC 4258. Six of the observed regions are located in the SE inner spiral arms and the other two are isolated in the northern outer arms.A detailed analysis of the physical conditions of the gas has been performed. For two of the regions an electron temperature has been derived from the [SIII] λ 6312Å line. For the rest, an empirical calibration based on the red and near infrared sulphur lines has been used. The oxygen abundances derived by both methods are found to be significantly lower (by a factor of two) than previously derived by using empirical calibrations based on the optical oxygen lines.In the brightest region, 74C, the observation of a prominent feature due to WolfRayet stars provides an excellent constraint over some properties of the ionizing clusters. In the light of the current evolutionary synthesis models, no consistent solution is found to explain at the same time both the WR feature characteristics and the emission line spectrum of this region. In principle, the presence of WR stars could lead to large temperature fluctuations and also to a hardening of the ionizing radiation. None of these effects are found in region 74C for which the electron temperatures found from the [SIII] λ 6312Å line and the Paschen discontinuity at 8200Å are equal within the errors and the effective temperature of the ionizing radiation is estimated at around 35300 K.Both more observations of confirmed high metallicity regions and a finer metallicity grid for the evolutionary synthesis models are needed in order to understand the ionizing populations of HII regions.

show abstract

“…We further normalised the spectrum and determined the equivalent widths (EWs) of all identified lines. Uncertainties were estimated from the EW and the root mean Article number, page 18 of 22 T.-W. Chen et al: The interacting host galaxy of the SLSN LSQ14mo square (rms) of the continuum according to the equation from Gonzalez-Delgado et al (1994):…”

Section: Appendix B: Emission Line Flux Measurementmentioning

confidence: 99%

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

Chen

Nicholl

Smartt

et al. 2017

A&A

View full text Add to dashboard Cite

We present and analyse an extensive dataset of the superluminous supernova (SLSN) LSQ14mo (z = 0.256), consisting of a multicolour lightcurve from −30 d to +70 d in the rest-frame (relative to maximum light) and a series of six spectra from PESSTO covering −7 d to +50 d. This is among the densest spectroscopic coverage, and best-constrained rising lightcurve, for a fast-declining hydrogenpoor SLSN. The bolometric lightcurve can be reproduced with a millisecond magnetar model with ∼ 4 M ejecta mass, and the temperature and velocity evolution is also suggestive of a magnetar as the power source. Spectral modelling indicates that the SN ejected ∼ 6 M of CO-rich material with a kinetic energy of ∼ 7 × 10 51 erg, and suggests a partially thermalised additional source of luminosity between −2 d and +22 d. This may be due to interaction with a shell of material originating from pre-explosion mass loss. We further present a detailed analysis of the host galaxy system of LSQ14mo. PESSTO and GROND imaging show three spatially resolved bright regions, and we used the VLT and FORS2 to obtain a deep (five-hour exposure) spectra of the SN position and the three star-forming regions, which are at a similar redshift. The FORS spectrum at +300 days shows no trace of SN emission lines and we place limits on the strength of [O i] from comparisons with other Ic supernovae. The deep spectra provides a unique chance to investigate spatial variations in the host star-formation activity and metallicity. The specific star-formation rate is similar in all three components, as is the presence of a young stellar population. However, the position of LSQ14mo exhibits a lower metallicity, with 12 + log(O/H) = 8.2 in both the R 23 and N2 scales (corresponding to ∼ 0.3 Z ). We propose that the three bright regions in the host system are interacting, which thus triggers star formation and forms young stellar populations.

show abstract

Violent star formation in NGC 2363

Cited by 134 publications

References 0 publications

The broad Hα, [O III] line wings in stellar supercluster A of NGC 2363 and the turbulent mixing layer hypothesis

The broad Hα, [O III] line wings in stellar supercluster A of NGC 2363 and the turbulent mixing layer hypothesis

Chemical abundances and ionizing clusters of H ii regions in the LINER galaxy NGC 4258

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

Contact Info

Product

Resources

About