Type Ia supernova host galaxies as seen with IFU spectroscopy

Stanishev, V.; Rodrigues, M.; Mourão, A.; Flores, H.

doi:10.1051/0004-6361/201219188

Cited by 28 publications

(43 citation statements)

References 137 publications

(256 reference statements)

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“…Observations of NGC 6754 were proposed for Science Verification of the instrument, and after a careful search in other commissioning and SV data, we put together a sample of 6 nearby galaxies that hosted 11 SNe (7 type II, 4 type Ia). Similar analysis was performed on MUSE datacubes as that in Stanishev et al (2012) and Galbany et al (2014), which previously analysed SN environments within the CALIFA survey. In this analysis we concentrated on extracting all possible Hii regions within host galaxies and then characterised the SN host Hii region within the context of all other Hii regions within each galaxy.…”

Section: Discussionmentioning

confidence: 91%

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Characterizing the environments of supernovae with MUSE

Galbany

Anderson

Rosales-Ortega

et al. 2015

Mon. Not. R. Astron. Soc.

130

125

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We present a statistical analysis of the environments of 11 supernovae (SNe) which occurred in 6 nearby galaxies (z 0.016). All galaxies were observed with MUSE, the high spatial resolution integral field spectrograph mounted to the 8m VLT UT4. These data enable us to map the full spatial extent of host galaxies up to ∼3 effective radii. In this way, not only can one characterise the specific host environment of each SN, one can compare their properties with stellar populations within the full range of other environments within the host. We present a method that consists of selecting all Hii regions found within host galaxies from 2D extinction-corrected Hα emission maps. These regions are then characterised in terms of their Hα equivalent widths, star formation rates, and oxygen abundances. Identifying Hii regions spatially coincident with SN explosion sites, we are thus able to determine where within the distributions of host galaxy e.g. metallicities and ages each SN is found, thus providing new constraints on SN progenitor properties. This initial pilot study using MUSE opens the way for a revolution in SN environment studies where we are now able to study multiple environment SN progenitor dependencies using a single instrument and single pointing.

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Section: Discussionmentioning

confidence: 91%

“…As noted in the introduction, we have previous experience of analysing wide-field IFS observations of SN host galaxies through the CALIFA survey (see SN environment analysis in Stanishev et al 2012 andGalbany et al 2014). Hence, the same techniques were adapted to MUSE data.…”

Section: Discussionmentioning

confidence: 99%

Characterizing the environments of supernovae with MUSE

Galbany

Anderson

Rosales-Ortega

et al. 2015

Mon. Not. R. Astron. Soc.

130

125

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“…We used the SSP model base of Bruzual (2007) and selected 66 models from it. This selection base has been applied in Stanishev et al (2012); Galbany et al (2014Galbany et al ( , 2016, which consists of 66 components with 17 different ages (from 1 Myr to 18 Gyr) and four metallicities (0.2, 0.4, 1.0 and 2.5 Z , where Z = 0.02) coming from a slightly modified version of the models of Bruzual & Charlot (2003) and uses a Chabrier (2003) IMF. In general, the model fittings are good for three components with a χ 2 of 2.22, 0.03, and 0.08 for positions A, B, and C, respectively.…”

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

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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.

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“…Given the much longer expected delay times of SNe Ia, interpreting environmental results becomes more difficult as progenitors have possibly travelled large distances before explosion. However, some intriguing re- Stanishev et al (2012) presented a first IFU study of SN host galaxies, analysing the spatial and spectral information obtained for a sample of six SNe Ia, and showing the capabilities of using such observations. Rigault et al (2013) also used IFU observations of a large sample of SN Ia host galaxies.…”

Section: Sn Ia Environmentsmentioning

confidence: 99%

Statistical Studies of Supernova Environments

Anderson

James

Habergham

et al. 2015

Publ. Astron. Soc. Aust.

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Mapping the diversity of supernovae (SNe) to progenitor properties is key to our understanding of stellar evolution and explosive stellar death. Investigations of the immediate environments of SNe allow statistical constraints to be made on progenitor properties such as mass and metallicity. Here we review the progress that has been made in this field. Pixel statistics using tracers of e.g. star formation within galaxies show intriguing differences in the explosion sites of, in particular SNe types II and Ibc (SNe II and SNe Ibc respectively), suggesting statistical differences in population ages. Of particular interest is that SNe Ic are significantly more associated with host galaxy Hα emission than SNe Ib, implying shorter lifetimes for the former. In addition, such studies have shown (unexpectedly) that the interacting SNe IIn do not explode in regions containing the most massive stars, which suggests that at least a significant fraction of their progenitors arise from the lower end of the core-collapse SN mass range. Host H ii region spectroscopy has been obtained for a significant number of core-collapse events, however definitive conclusions on differences between distinct SN types have to-date been elusive. Single stellar evolution models predict that the relative fraction of SNe Ibc to SNe II should increase with increasing metallicity, due to the dependence of mass-loss rates on progenitor metallicity. We present a meta-analysis of all current host H ii region oxygen abundances for CC SNe. It is concluded that the SN II to SN Ibc ratio shows little variation with oxygen abundance, with only a suggestion that the ratio increases in the lowest bin. Radial distributions of different SNe are discussed, where a central excess of SNe Ibc has been observed within disturbed galaxy systems, which is difficult to ascribe to metallicity or selection effects. Environment studies are also being undertaken for SNe Ia, where constraints can be made on the shortest delay times of progenitor systems. It is shown that 'redder' SNe Ia are more often found within star-forming regions. Environment studies are evolving to enable studies at higher spatial resolutions than previously possible, while in addition the advent of widefield integral field unit instruments allows galaxy-wide spectral analyses which will provide fruitful results to this field. Some example contemporary results are shown in that direction.

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Type Ia supernova host galaxies as seen with IFU spectroscopy

Cited by 28 publications

References 137 publications

Characterizing the environments of supernovae with MUSE

Characterizing the environments of supernovae with MUSE

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

Statistical Studies of Supernova Environments

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