scholarly journals The SLUGGS Survey: A New Mask Design to Reconstruct the Stellar Populations and Kinematics of Both Inner and Outer Galaxy Regions

2016 ◽  
Vol 33 ◽  
Author(s):  
Nicola Pastorello ◽  
Duncan A. Forbes ◽  
Adriano Poci ◽  
Aaron J. Romanowsky ◽  
Richard McDermid ◽  
...  
Keyword(s):  
Spatial Scales ◽  
Stellar Populations ◽  
Large Field ◽  
Nearby Galaxy ◽  
Stellar Kinematics ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Mask Design ◽  
Field Unit ◽  
Integral Field

AbstractIntegral field unit spectrographs allow the 2D exploration of the kinematics and stellar populations of galaxies, although they are generally restricted to small fields-of-view. Using the large field-of-view of the DEIMOS multislit spectrograph on Keck and our Stellar Kinematics using Multiple Slits technique, we are able to extract sky-subtracted stellar light spectra to large galactocentric radii. Here, we present a new DEIMOS mask design named SuperSKiMS that explores large spatial scales without sacrificing high spatial sampling. We simulate a set of observations with such a mask design on the nearby galaxy NGC 1023, measuring stellar kinematics and metallicities out to where the galaxy surface brightness is orders of magnitude fainter than the sky. With this technique we also reproduce the results from literature integral field spectroscopy in the innermost galaxy regions. In particular, we use the simulated NGC 1023 kinematics to model its total mass distribution to large radii, obtaining comparable results with those from published integral field unit observation. Finally, from new spectra of NGC 1023, we obtain stellar 2D kinematics and metallicity distributions that show good agreement with integral field spectroscopy results in the overlapping regions. In particular, we do not find a significant offset between our Stellar Kinematics using Multiple Slits and the ATLAS3D stellar velocity dispersion at the same spatial locations.

scholarly journals Stellar Populations of Brightest Cluster Galaxies and Intracluster Light

2016 ◽  
Vol 11 (S321) ◽  
pp. 193-195
Author(s):  
Louise O. V. Edwards ◽  
Isabella L. Trierweiller
Keyword(s):  
Stellar Populations ◽  
Population Synthesis ◽  
Cluster Galaxies ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Brightest Cluster Galaxies ◽  
Intracluster Light ◽  
Integral Field ◽  
Cluster Processes

AbstractWe present 3 representative cases from a sample of 16 local Brightest Cluster Galaxies observed using integral field spectroscopy. The observations extend to nearby neighbours and into the Intracluster Light (ICL). Population synthesis modeling shows that the ICL is younger and more metal poor compared to the BCG core and outskirts. This is consistent with a scenario in which the ICL grows by cluster processes, and alongside the growth of the BCG.

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.

scholarly journals Inflows and Outflows in Nearby AGN from Integral Field Spectroscopy

2009 ◽  
Vol 5 (S267) ◽  
pp. 290-298 ◽  
Author(s):  
Thaisa Storchi-Bergmann
Keyword(s):  
Near Infrared ◽  
Stellar Kinematics ◽  
Gas Emission ◽  
Ionized Gas ◽  
Integral Field Spectroscopy ◽  
Near Ir ◽  
Field Spectroscopy ◽  
The Galaxy ◽  
Mass Outflow ◽  
Integral Field

AbstractI report recent results on the kinematics of the inner few hundred parsecs (pc) around nearby active galactic nuclei (AGN) at a sampling of a few pc to a few tens of pc, using optical and near-infrared (near-IR) integral field spectroscopy obtained with the Gemini telescopes. The stellar kinematics of the hosts — comprised mostly of spiral galaxies — are dominated by circular rotation in the plane of the galaxy. Inflows with velocities of ~50 km s−1 have been observed along nuclear spiral arms in (optical) ionized gas emission for low-luminosity AGN and in (near-IR) molecular gas emission for higher-luminosity AGN. We have also observed gas rotating in the galaxy plane, sometimes in compact (few tens of pc) disks which may be fuelling the AGN. Outflows have been observed mostly in ionized gas emission from the narrow-line region, whose flux distributions and kinematics frequently correlate with radio flux distributions. Channel maps along the emission-line profiles reveal velocities as high as ~ 600 km s−1. Mass outflow rates in ionized gas range from 10−2 to 10−3M⊙ yr−1 and are 10–100 times larger than the mass accretion rates on to the AGN, supporting an origin for the bulk of the outflow in gas from the galaxy plane entrained by a nuclear jet or accretion disk wind.

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 Resolving stellar populations with integral field spectroscopy

2019 ◽  
Vol 340 (9-10) ◽  
pp. 989-995
Author(s):  
Martin M. Roth ◽  
Peter M. Weilbacher ◽  
Norberto Castro
Keyword(s):  
Stellar Populations ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field

Feedback from ionised gas outflows in the central kpc of nearby active galaxies

2020 ◽  
Vol 15 (S359) ◽  
pp. 267-268
Author(s):  
Edwin David ◽  
Thaisa Storchi-Bergmann
Keyword(s):  
Active Galaxies ◽  
Feedback Effect ◽  
Host Galaxies ◽  
Gas Distribution ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Mass Outflow ◽  
Field Unit ◽  
Integral Field

AbstractWe use integral-field spectroscopy obtained with the Gemini instrument GMOS-IFU (Gemini Multi-Object Spectrograph Integral Field Unit) to map the gas distribution, excitation and kinematics in the central kpc of 11 nearby active galaxies. We use channel maps to quantify the ionised gas masses, mass outflow rates and powers of the outflows in order to gauge the feedback effect of these outflows on the host galaxies. We compare this method with others previously used to calculate the feedback power of such outflows.

scholarly journals Integral field spectroscopy of Green Peas – I. Disentangling disc-like turbulence and strong outflow kinematics in SDSS J083843.63+385350.5

2019 ◽  
Vol 489 (2) ◽  
pp. 1787-1796 ◽  
Author(s):  
G Bosch ◽  
G F Hägele ◽  
R Amorín ◽  
V Firpo ◽  
M V Cardaci ◽  
...  
Keyword(s):  
Emission Line ◽  
Large Scale ◽  
Formation Rate ◽  
Mixing Layer ◽  
Line Profiles ◽  
Statistical Indicator ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Field Unit ◽  
Integral Field

ABSTRACT Integral field spectroscopy is well known for providing detailed insight of extended sources thanks to the possibility of handling space resolved spectroscopic information. Simple and straightforward analysis such as single line fitting yields interesting results, although it might miss a more complete picture in many cases. Violent star-forming regions, such as starburst galaxies, display very complex emission line profiles due to multiple kinematic components superposed in the line of sight. We perform a spatially resolved kinematical study of a single Green Pea (GP) galaxy, SDSS J083843.63+385350.5, using a new method for analysing integral field unit observations of emission line spectra. The method considers the presence of multiple components in the emission line profiles and makes use of a statistical indicator to determine the meaningful number of components to fit the observed profiles. We are able to identify three distinct kinematic features throughout the field and discuss their link with a rotating component, a strong outflow, and a turbulent mixing layer. We also derive an updated star formation rate for SDSS J0838 and discuss the link between the observed signatures of a large-scale outflow and of the Lyman continuum leakage detected in GP galaxies.

scholarly journals A MUSE study of the fast bar in the weakly-interacting galaxy NGC 4264

2019 ◽  
Vol 14 (S353) ◽  
pp. 172-175
Author(s):  
Virginia Cuomo ◽  
Enrico Maria Corsini ◽  
Alfonso J. L. Aguerri ◽  
Victor P. Debattista
Keyword(s):  
Rotation Rate ◽  
Virgo Cluster ◽  
Surface Photometry ◽  
Stellar Kinematics ◽  
Tidal Interaction ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Weakly Interacting ◽  
Pattern Speed ◽  
Integral Field

AbstractWe present surface photometry and stellar kinematics of NGC 4264, a lenticular galaxy in the region of the Virgo Cluster undergoing a tidal interaction with its neighbour, NGC 4261. We measured the bar radius and strength from SDSS imaging and the bar pattern speed from MUSE integral-field spectroscopy. We find that NGC 4264 hosts a strong and large bar, which is rotating fast. The accurate measurement of the bar rotation rate allows us to exclude that the formation of the bar was triggered by the ongoing interaction.

scholarly journals Uncertainties in gas kinematics arising from stellar continuum modeling in integral field spectroscopy data: the case of NGC 2906 observed with VLT/MUSE

2019 ◽  
Vol 625 ◽  
pp. A83 ◽  
Author(s):  
E. Bellocchi ◽  
Y. Ascasibar ◽  
L. Galbany ◽  
S. F. Sánchez ◽  
H. Ibarra–Medel ◽  
...  
Keyword(s):  
Nearby Galaxy ◽  
Ionization Mechanisms ◽  
Gas Kinematics ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Very Large Telescope ◽  
Galaxy Kinematics ◽  
Instrumental Resolution ◽  
Line Fitting ◽  
Integral Field

Context. Integral field spectroscopy (IFS) provides detailed information about galaxy kinematics at high spatial and spectral resolution, and the disentanglement of the gaseous and stellar components is a key step in the analysis of the data. Aims. We study how the use of several stellar-subtraction methods and line fitting approaches can affect the derivation of the main kinematic parameters (velocity and velocity dispersion fields) of the ionized gas component. Methods. The target of this work is the nearby galaxy NGC 2906, observed with the MUSE instrument at the Very Large Telescope (VLT). A sample of twelve spectra is selected from the inner (nucleus) and outer (spiral arms) regions, characterized by different ionization mechanisms. We compare three different methods to subtract the stellar continuum (FIT3D, STARLIGHT and pPXF), combined with one of the following stellar libraries: MILES, STELIB and GRANADA+MILES. Results. The choice of the stellar-subtraction method is the most important ingredient affecting the derivation of the gas kinematics, followed by the choice of the stellar library and by the line-fitting approach. In our data, typical uncertainties in the observed wavelength and width of the Hα and [NII] lines are of the order of ⟨δλ⟩rms ∼ 0.1 Å and ⟨δσ⟩rms ∼ 0.2 Å (i.e., ∼5 and 10 km s−1, respectively). The results obtained from the [NII] line seem to be slightly more robust, as it is less affected by stellar absorption than Hα. All methods considered yield statistically consistent measurements once a mean systemic contribution Δλ¯ = Δσ¯ = 0.2 ΔMUSE is added in quadrature to the line-fitting errors, where ΔMUSE = 1.1 Å ∼50 km s−1, which denotes the instrumental resolution of the MUSE spectra. Conclusions. Although the subtraction of the stellar continuum is critical in order to recover line fluxes, any method (including none) can be used to measure the gas kinematics, as long as an additional component, Δλ¯ = Δσ¯ = 0.2 ΔMUSE, is added to the error budget.

scholarly journals Stellar populations in bulges and disks and the secular evolution connection

2012 ◽  
Vol 10 (H16) ◽  
pp. 336-336
Author(s):  
Reynier Peletier
Keyword(s):  
Stellar Populations ◽  
Secular Evolution ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Central Regions ◽  
Integral Field

AbstractIn recent years a considerable amount of new data has become available about stellar populations in the central regions of galaxies. I will discuss what stellar populations can tell us about the formation origin of bulges, and how this relates to the formation of the central regions in giant and dwarf ellipticals. In particular I will concentrate on results from integral field spectroscopy and Spitzer imaging at 3.6, 4.5 and 8 microns.

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