Mass and metallicity constraints on supernova progenitors derived from integral field spectroscopy of the environment

2011 ◽  
Vol 7 (S279) ◽  
pp. 343-344
Author(s):  
Hanindyo Kuncarayakti ◽  
Mamoru Doi ◽  
Greg Aldering ◽  
Nobuo Arimoto ◽  
Keiichi Maeda ◽  
...  
Keyword(s):  
Stellar Population ◽  
Star Cluster ◽  
Initial Mass ◽  
Strong Line ◽  
Reliable Determination ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Progenitor Stars ◽  
Integral Field

AbstractWe have obtained optical integral field spectroscopy of the explosion sites of more than 25 nearby type-IIP/IIL/Ib/Ic supernovae using UH88/SNIFS, and additionally Gemini/GMOS IFU. This technique enables us to obtain both spatial and spectral information of the immediate environment of the supernovae. Using strong line method we measured the metallicity of the star cluster present at the explosion site, presumably the coeval parent stellar population of the supernova progenitor, and comparison with simple stellar population models gives age estimate of the cluster. With this method we were able to put constraints on the metallicity and age of the progenitor star. The age, i.e. lifetime, of the progenitor corresponds to the initial mass of the star. By far this is the most direct measurement of supernova progenitor metallicity and, if the cluster-progenitor association is confirmed, provides reliable determination of the initial mass of supernova progenitor stars.

scholarly journals Constraints on core-collapse supernova progenitors from explosion site integral field spectroscopy

2018 ◽  
Vol 613 ◽  
pp. A35 ◽  
Author(s):  
H. Kuncarayakti ◽  
J. P. Anderson ◽  
L. Galbany ◽  
K. Maeda ◽  
M. Hamuy ◽  
...  
Keyword(s):  
Stellar Population ◽  
Near Infrared ◽  
Stellar Populations ◽  
Star Formation History ◽  
Initial Mass ◽  
Strong Line ◽  
Core Collapse ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field

Context. Observationally, supernovae (SNe) are divided into subclasses according to their distinct characteristics. This diversity naturally reflects the diversity in the progenitor stars. It is not entirely clear, however, how different evolutionary paths leading massive stars to become an SN are governed by fundamental parameters such as progenitor initial mass and metallicity. Aims. This paper places constraints on progenitor initial mass and metallicity in distinct core-collapse SN subclasses through a study of the parent stellar populations at the explosion sites. Methods. Integral field spectroscopy (IFS) of 83 nearby SN explosion sites with a median distance of 18 Mpc has been collected and analysed, enabling detection and spectral extraction of the parent stellar population of SN progenitors. From the parent stellar population spectrum, the initial mass and metallicity of the coeval progenitor are derived by means of comparison to simple stellar population models and strong-line methods. Additionally, near-infrared IFS was employed to characterise the star formation history at the explosion sites. Results. No significant metallicity differences are observed among distinct SN types. The typical progenitor mass is found to be highest for SN type Ic, followed by type Ib, then types IIb and II. Type IIn is the least associated with young stellar populations and thus massive progenitors. However, statistically significant differences in progenitor initial mass are observed only when comparing SNe IIn with other subclasses. Stripped-envelope SN progenitors with initial mass estimates lower than 25 M⊙ are found; they are thought to be the result of binary progenitors. Confirming previous studies, these results support the notion that core-collapse SN progenitors cannot arise from single-star channels only, and both single and binary channels are at play in the production of core-collapse SNe. Near-infrared IFS suggests that multiple stellar populations with different ages may be present in some of the SN sites. As a consequence, there could be a non-negligible amount of contamination from old populations, and therefore the individual age estimates are effectively lower limits.

scholarly journals The explosion sites of nearby supernovae seen with integral field spectroscopy

2015 ◽  
Vol 11 (A29B) ◽  
pp. 276-277
Author(s):  
Hanindyo Kuncarayakti
Keyword(s):  
Stellar Population ◽  
Near Infrared ◽  
Spectral Information ◽  
Physical Parameters ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Different Types ◽  
Optical Wavelengths ◽  
Integral Field

AbstractIntegral field spectroscopy of nearby supernova sites within ~30 Mpc have been obtained using multiple IFU spectrographs in Hawaii and Chile. This technique enables both spatial and spectral information of the explosion sites to be acquired simultaneously, thus providing the identification of the parent stellar population of the supernova progenitor and the estimates for its physical parameters including age and metallicity via the spectrum. While this work has mainly been done in the optical wavelengths using instruments such as VIMOS, GMOS, and MUSE, a near-infrared approach has also been carried out using the AO-assisted SINFONI. By studying the supernova parent stellar population, we aim to characterize the mass and metallicity of the progenitors of different types of supernovae.

scholarly journals Properties of the HII Regions Derived Using Integral Field Spectroscopy

2013 ◽  
Vol 2013 ◽  
pp. 1-14 ◽  
Author(s):  
Sebastian F. Sánchez
Keyword(s):  
Stellar Population ◽  
Mass Density ◽  
Disk Galaxies ◽  
Orion Nebula ◽  
Chemical Enrichment ◽  
Large Samples ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Inside Out ◽  
Integral Field

Here we review some of our more recent results on the observed properties of HIIregions using Integral Field Spectroscopy. In particular, we illustrate the use of this technique to study in detail the ionization conditions across the nebulae for galactic HIIregions (focused on the Orion Nebula) and the statistical study of large samples of extragalactic HIIregions. We review the reported new scaling relation between the local mass density and the oxygen abundance across the disk galaxies and the recently discovered universal gradient for oxygen abundances. We update our previous results the lack of a dependence of the Mass-Metallicity relation with the starformation rate, including new unpublished data. Finally we discuss on the relation between the ionization conditions in the nebulae and the underlying stellar population. All together our results indicate that disk galaxies present a chemical enrichment dominated by an inside-out growth scenario, with a less evident effect of radial migrations and/or outflows.

scholarly journals Are Wolf-Rayet Stars Able to Pollute the Interstellar Medium of Galaxies? Results from Integral Field Spectroscopy

2013 ◽  
Vol 2013 ◽  
pp. 1-15 ◽  
Author(s):  
Enrique Pérez-Montero ◽  
Carolina Kehrig ◽  
Jarle Brinchmann ◽  
José M. Vílchez ◽  
Daniel Kunth ◽  
...  
Keyword(s):  
Direct Method ◽  
Spatial Scales ◽  
Strong Line ◽  
Chemical Abundances ◽  
Local Pollution ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Low Surface Brightness ◽  
Low Metallicity ◽  
Integral Field

We investigate the spatial distribution of chemical abundances in a sample of low metallicity Wolf-Rayet (WR) galaxies selected from the SDSS. We used the integral field spectroscopy technique in the optical spectral range (3700 Å–6850 Å) with PMAS attached to the CAHA 3.5 m telescope. Our statistical analysis of the spatial distributions of O/H and N/O, as derived using the direct method or strong-line parameters consistent with it, indicates that metallicity is homogeneous in five out of the six analysed objects in scales of the order of several kpc. Only in the object WR404 is a gradient of metallicity found in the direction of the low surface brightness tail. In contrast, we found an overabundance of N/O in spatial scales of the order of hundreds of pc associated with or close to the positions of the WR stars in 4 out of the 6 galaxies. We exclude possible hydrodynamical causes, such as the metal-poor gas inflow, for this local pollution by means of the analysis of the mass-metallicity relation (MZR) and mass-nitrogen-to-oxygen relation (MNOR) for the WR galaxies catalogued in the SDSS.

Integral field spectroscopy with GEMINI: Extragalactic star cluster in NGC1275

2006 ◽  
Vol 49 (10-12) ◽  
pp. 613-617 ◽  
Author(s):  
Gelys Trancho ◽  
Bryan Miller ◽  
Begoña García-Lorenzo ◽  
Sebastián F. Sánchez
Keyword(s):  
Star Cluster ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field

scholarly journals Key dynamical results from the SAMI Galaxy Survey

2019 ◽  
Vol 14 (S353) ◽  
pp. 213-221
Author(s):  
Jesse van de Sande ◽  
Joss Bland-Hawthorn ◽  
Dilyar Barat ◽  
Sarah Brough ◽  
Julia J. Bryant ◽  
...  
Keyword(s):  
Angular Momentum ◽  
Stellar Population ◽  
Stellar Mass ◽  
Two Dimensional ◽  
Physical Processes ◽  
Spatially Resolved ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Gas Measurements ◽  
Integral Field

AbstractWe present an overview of recent key results from the SAMI Galaxy Survey on the build-up of mass and angular momentum in galaxies across morphology and environment. The SAMI Galaxy survey is a multi-object integral field spectroscopic survey and provides a wealth of spatially-resolved, two-dimensional stellar and gas measurements for galaxies of all morphological types, with high-precision due the stable spectral resolution of the AAOmega spectrograph. The sample size of ~3000 galaxies allows for dividing the sample in bins of stellar mass, environment, and star-formation or morphology, whilst maintaining a statistical significant number of galaxies in each bin. By combining imaging, spatially resolved dynamics, and stellar population measurements, our result demonstrate the power of utilising integral field spectroscopy on a large sample of galaxies to further our understanding of physical processes involved in the build-up of stellar mass and angular momentum in galaxies.

scholarly journals Supermassive black holes from OASIS and SAURON integral-field kinematics

2007 ◽  
Vol 3 (S245) ◽  
pp. 215-218 ◽  
Author(s):  
Michele Cappellari ◽  
R. Bacon ◽  
Roger L. Davies ◽  
P. T. de Zeeuw ◽  
Eric Emsellem ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Supermassive Black Holes ◽  
Modeling Effort ◽  
The Past ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Black Hole Masses ◽  
Integral Field

AbstractSupermassive black holes are a key element in our understanding of how galaxies form. Most of the progress in this very active field of research is based on just ~30 determination of black hole masses, accumulated over the past decade. We illustrate how integral-field spectroscopy, and in particular our OASIS modeling effort can help improve the current situation.

scholarly journals The stellar structure of early-type galaxies: a wide-field Mitchell Spectrograph view

2016 ◽  
Vol 11 (S321) ◽  
pp. 288-288
Author(s):  
N. F. Boardman ◽  
A. Weijmans ◽  
R. C. E. van den Bosch ◽  
L. Zhu ◽  
A. Yildirim ◽  
...  
Keyword(s):  
Effective Radius ◽  
Stellar Structure ◽  
Wide Field ◽  
Early Type ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field ◽  
Made In

Much progress has been made in recent years towards understanding how early-type galaxies (ETGs) form and evolve. SAURON (Bacon et al. 2001) integral-field spectroscopy from the ATLAS3D survey (Cappellari et al. 2011) has suggested that less massive ETGs are linked directly to spirals, whereas the most massive objects appear to form from a series of merging and accretion events (Cappellari et al. 2013). However, the ATLAS3D data typically only extends to about one half-light radius (or effective radius, Re), making it unclear if this picture is truly complete.

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