Spectroscopy of superluminous supernova host galaxies. A preference of hydrogen-poor events for extreme emission line galaxies

Leloudas, G.; Schulze, S.; Krühler, T.; Gorosabel, J.; Christensen, L.; Mehner, A.; Postigo, A. de Ugarte; Amorín, R.; Thöne, C. C.; Anderson, J. P.; Bauer, F. E.; Gallazzi, Anna; Hełminiak, K. G.; Hjorth, J.; Ibar, E.; Malesani, D.; Morrell, N.; Vinkó, J.; Wheeler, J. C.

doi:10.1093/mnras/stv320

Cited by 222 publications

(355 citation statements)

References 154 publications

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“…This characteristic of SLSN host galaxies has been noticed in Leloudas et al (2015b), and the host galaxy of LSQ14mo (position C) also follows this trend.…”

Section: Gas-phase Metallicity Of the Host Galaxysupporting

confidence: 70%

“…However, this is not corroborated by the Hubble Space Telescope study of hosts by Lunnan et al (2015). There is no significant difference in host environments of fast-declining and slowly-fading SLSNe Leloudas et al 2015b;Perley et al 2016). Recently, Perley et al (2016) and Chen et al (2016) both suggested that a sub-solar metallicity is required for SLSN progenitors.…”

Section: Introductionmentioning

confidence: 92%

“…The host galaxies of SLSNe are generally faint dwarf galaxies (Neill et al 2011) which tend to have low metallicity and low mass (Stoll et al 2011;Chen et al 2013;Lunnan et al 2013). They share properties with LGRB host galaxies (Lunnan et al 2014;Japelj et al 2016), although SLSN host galaxies appear more extreme (Vreeswijk et al 2014;Chen et al 2015;Leloudas et al 2015b;Angus et al 2016). Leloudas et al (2015b) found that the equivalent widths of [O iii] are much higher in SLSN hosts than in LGRB hosts, which they argue may imply that the stellar population is, on average, younger in SLSN than in LGRB host galaxies, and by implication that the progenitors of SLSNe are more massive than GRBs.…”

Section: Introductionmentioning

confidence: 99%

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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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“…This characteristic of SLSN host galaxies has been noticed in Leloudas et al (2015b), and the host galaxy of LSQ14mo (position C) also follows this trend.…”

Section: Gas-phase Metallicity Of the Host Galaxysupporting

confidence: 70%

Section: Introductionmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

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

Chen

Nicholl

Smartt

et al. 2017

A&A

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“…These properties make them unique probes with which to study the details of chemical enrichment, massive star formation, and feedback processes in galaxies with physical properties (i.e., size, mass, SFR, metallicity, gas, and dust relative content) most closely resembling those prevailing at high redshift, e.g., Lyman-break galaxies and Lyman-α emitters (e.g., Pettini et al 2001;Finkelstein et al 2011). Furthermore, increasing observational evidence point to EELGs as the likely environments to host the progenitors of long-duration gamma-ray bursts (e.g., Christensen et al 2004;Kewley et al 2007;Savaglio et al 2009;Guseva et al 2011) and the most luminous supernovae (Chen et al 2013;Lunnan et al 2013;Leloudas et al 2015;Thöne et al 2014).…”

Section: Introductionmentioning

confidence: 94%

Extreme emission-line galaxies out toz~ 1 in zCOSMOS

Amorín

Pérez-Montero

Contini

et al. 2015

A&A

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113

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Context. The study of large and representative samples of low-metallicity star-forming galaxies at different cosmic epochs is of great interest to the detailed understanding of the assembly history and evolution of low-mass galaxies. Aims. We present a thorough characterization of a large sample of 183 extreme emission-line galaxies (EELGs) at redshift 0.11 ≤ z ≤ 0.93 selected from the 20k zCOSMOS bright survey because of their unusually large emission line equivalent widths. Methods. We use multiwavelength COSMOS photometry, HST-ACS I-band imaging, and optical zCOSMOS spectroscopy to derive the main global properties of star-forming EELGs, such as sizes, stellar masses, star formation rates (SFR), and reliable oxygen abundances using both "direct" and "strong-line" methods. Results. The EELGs are extremely compact (r 50 ∼ 1.3 kpc), low-mass (M * ∼ 10 7 −10 10 M ) galaxies forming stars at unusually high specific star formation rates (sSFR ≡ SFR/M up to 10 −7 yr −1 ) compared to main sequence star-forming galaxies of the same stellar mass and redshift. At rest-frame UV wavelengths, the EELGs are luminous and show high surface brightness and include strong Lyα emitters, as revealed by GALEX spectroscopy. We show that zCOSMOS EELGs are high-ionization, low-metallicity systems, with median 12+ log(O/H) = 8.16 ± 0.21 (0.2 Z ) including a handful of extremely metal-deficient (<0.1 Z ) EELGs. While ∼80% of the EELGs show non-axisymmetric morphologies, including clumpy and cometary or tadpole galaxies, we find that ∼29% of them show additional low-surface-brightness features, which strongly suggests recent or ongoing interactions. As star-forming dwarfs in the local Universe, EELGs are most often found in relative isolation. While only very few EELGs belong to compact groups, almost one third of them are found in spectroscopically confirmed loose pairs or triplets. Conclusions. The zCOSMOS EELGs are galaxies caught in a transient and probably early period of their evolution, where they are efficiently building up a significant fraction of their present-day stellar mass in an ongoing, galaxy-wide starburst. Therefore, the EELGs constitute an ideal benchmark for comparison studies between low-and high-redshift low-mass star-forming galaxies.

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“…A variety of other mechanisms can mimic the properties of AGN in these diagnostics, such as shocks, supernovae, and their subsequent remnants. Indeed, SFDGs (and in particular EELGs) appear to be the preferred sites for the most powerful supernova explosions (Chen et al 2013;Lunnan et al 2013;Leloudas et al 2015;Thöne et al 2015).…”

Section: Identification Of Agns: Diagnostic Diagramsmentioning

confidence: 99%

Characterization of star-forming dwarf galaxies at 0.1 ≲z ≲ 0.9 in VUDS: probing the low-mass end of the mass-metallicity relation

Calabró

Amorín

Fontana

et al. 2017

A&A

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Context. The study of statistically significant samples of star-forming dwarf galaxies (SFDGs) at different cosmic epochs is essential for the detailed understanding of galaxy assembly and chemical evolution. However, the main properties of this large population of galaxies at intermediate redshift are still poorly known. Aims. We present the discovery and spectrophotometric characterization of a large sample of 164 faint (i AB ∼ 23-25 mag) SFDGs at redshift 0.13 ≤ z ≤ 0.88 selected by the presence of bright optical emission lines in the VIMOS Ultra Deep Survey (VUDS). We investigate their integrated physical properties and ionization conditions, which are used to discuss the low-mass end of the mass-metallicity relation (MZR) and other key scaling relations. Methods. We use optical VUDS spectra in the COSMOS, VVDS-02h, and ECDF-S fields, as well as deep multi-wavelength photometry that includes HST-ACS F814W imaging, to derive stellar masses, extinction-corrected star-formation rates (SFR), and gas-phase metallicities of SFDGs. For the latter, we use the direct method and a T e -consistent approach based on the comparison of a set of observed emission lines ratios with the predictions of detailed photoionization models. Results. The VUDS SFDGs are compact (median r e ∼ 1.2 kpc), low-mass (M * ∼ 10 7 -10 9 M ) galaxies with a wide range of starformation rates (SFR(Hα) ∼ 10 −3 -10 1 M /yr) and morphologies. Overall, they show a broad range of subsolar metallicities (12 + log(O/H) = 7.26-8.7; 0.04 < ∼ Z/Z < ∼ 1). Nearly half of the sample are extreme emission-line galaxies (EELGs) characterized by high equivalent widths and emission line ratios indicative of higher excitation and ionization conditions. The MZR of SFDGs shows a flatter slope compared to previous studies of galaxies in the same mass range and redshift. We find the scatter of the MZR is partly explained in the low mass range by varying specific SFRs and gas fractions amongst the galaxies in our sample. In agreement with recent studies, we find the subclass of EELGs to be systematically offset to lower metallicity compared to SFDGs at a given stellar mass and SFR, suggesting a younger starburst phase. Compared with simple chemical evolution models we find that most SFDGs do not follow the predictions of a "closed-box" model, but those from a gas-regulating model in which gas flows are considered. While strong stellar feedback may produce large-scale outflows favoring the cessation of vigorous star formation and promoting the removal of metals, younger and more metal-poor dwarfs may have recently accreted large amounts of fresh, very metal-poor gas, that is used to fuel current star formation.

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Spectroscopy of superluminous supernova host galaxies. A preference of hydrogen-poor events for extreme emission line galaxies

Cited by 222 publications

References 154 publications

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

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

Extreme emission-line galaxies out toz~ 1 in zCOSMOS

Characterization of star-forming dwarf galaxies at 0.1 ≲z ≲ 0.9 in VUDS: probing the low-mass end of the mass-metallicity relation

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