scholarly journals PPAK Wide field Integral Field Spectroscopy of NGC 628 – III. Stellar population properties

2013 ◽  
Vol 437 (2) ◽  
pp. 1534-1548 ◽  
Author(s):  
P. Sánchez-Blázquez ◽  
F. Rosales-Ortega ◽  
A. Diaz ◽  
S. F. Sánchez
Keyword(s):  
Stellar Population ◽  
Wide Field ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field ◽  
Field Integral

scholarly journals PPAK Wide-field Integral Field Spectroscopy of NGC 628 - I. The largest spectroscopic mosaic on a single galaxy★

2010 ◽  
Vol 410 (1) ◽  
pp. 313-340 ◽  
Author(s):  
S. F. Sánchez ◽  
F. F. Rosales-Ortega ◽  
R. C. Kennicutt ◽  
B. D. Johnson ◽  
A. I. Diaz ◽  
...  
Keyword(s):  
Wide Field ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field ◽  
Field Integral

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.

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 Imaging FTS: A Different Approach to Integral Field Spectroscopy

2014 ◽  
Vol 2014 ◽  
pp. 1-15 ◽  
Author(s):  
Laurent Drissen ◽  
Laurie Rousseau-Nepton ◽  
Sébastien Lavoie ◽  
Carmelle Robert ◽  
Thomas Martin ◽  
...  
Keyword(s):  
Fourier Transform ◽  
Emission Line ◽  
Absorption Line ◽  
Spiral Galaxy ◽  
Hyperspectral Imagery ◽  
Fourier Transform Spectroscopy ◽  
Wide Field ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field

Imaging Fourier transform spectroscopy (iFTS) is a promising, although technically very challenging, option for wide-field hyperspectral imagery. We present in this paper an introduction to the iFTS concept and its advantages and drawbacks, as well as examples of data obtained with a prototype iFTS, SpIOMM, attached to the 1.6 m telescope of the Observatoire du Mont-Mégantic: emission line ratios in the spiral galaxy NGC 628 and absorption line indices in the giant elliptical M87. We conclude by introducing SpIOMM's successor, SITELLE, which will be installed at the Canada-France-Hawaii Telescope in 2014.

scholarly journals Orientation of galactic bulge planetary nebulae toward the Galactic center

2014 ◽  
Vol 10 (S312) ◽  
pp. 128-130
Author(s):  
Ashkbiz Danehkar ◽  
Quentin A. Parker
Keyword(s):  
Emission Line ◽  
Galactic Center ◽  
Planetary Nebulae ◽  
Wide Field ◽  
Spatially Resolved ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
National University ◽  
Hα Emission ◽  
Integral Field

AbstractWe have used the Wide Field Spectrograph on the Australian National University 2.3-m telescope to perform the integral field spectroscopy for a sample of the Galactic planetary nebulae. The spatially resolved velocity distributions of the Hα emission line were used to determine the kinematic features and nebular orientations. Our findings show that some bulge planetary nebulae toward the Galactic center have a particular orientation.

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.

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.

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