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

Bellocchi, E.; Ascasíbar, Y.; Galbany, L.; Sánchez, S. F.; Ibarra-Medel, H.; Gavilán, M.; Díaz, Ángeles I.

doi:10.1051/0004-6361/201834478

Cited by 6 publications

(4 citation statements)

References 68 publications

(58 reference statements)

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“…So far it comprises ∼328 galaxies, being the core of the current compilation. This sample has been used to explore different science topics: (i) the radial profiles of the oxygen abundances in galaxies (Sánchez-Menguiano et al 2018), and its azimuthal variation (Sánchez et al 2015;Sánchez-Menguiano et al 2016); (ii) extended ionized gas fillaments associated to galaxy interactions (Prieto et al 2016a); (iii) the discovery of new strong lenses (Galbany et al 2018), and the optical counterpart of a radio-jet (López-Cobá et al 2017a); (iv) the derivation of main galaxy kinematic parameters such as velocity and velocity dispersion by different approaches (Bellocchi et al 2019); (v) individual type II supernova (Meza et al 2019); (vi) ionized gas tails (Boselli et al 2018); besides (vi) the local environment of supernovae, i.e., the major goal of the survey (Galbany et al 2016;Krühler et al 2017).…”

Section: The Amusing++ Samplementioning

confidence: 99%

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

López-Cobá¹,

Sánchez²,

Anderson

et al. 2020

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We present here AMUSING++; the largest compilation of nearby galaxies observed with the MUSE integral field spectrograph so far. This collection consists of 635 galaxies from different MUSE projects covering the redshift interval 0.0002 < z < 0.1. The sample and its main properties are characterized and described in here. It includes galaxies of almost all morphological types, with a good coverage in the color-magnitude diagram, within the stellar mass range between 10 8 to 10 12 M , and with properties resembling those of a diameter-selected sample. The AMUSING++ sample is therefore suitable to study, with unprecendent detail, the properties of nearby galaxies at global and local scales, providing us with more than 50 million individual spectra. We use this compilation to investigate the presence of galactic outflows. We exploit the use of combined emission-line images to explore the shape of the different ionized components and the distribution along classical diagnostic diagrams to disentangle the different ionizing sources across the optical extension of each galaxy. We use the cross correlation function to estimate the level of symmetry of the emission lines as an indication of the presence of shocks and/or active galactic nuclei. We uncovered a total of 54 outflows, comprising ∼8% of the sample. A large number of the discovered outflows correspond to those driven by active galactic nuclei (∼60%), suggesting some bias in the selection of our sample. No clear evidence was found that outflow host galaxies are highly star-forming, and outflows appear to be found within all galaxies around the star formation sequence.

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Section: The Amusing++ Samplementioning

confidence: 99%

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

López-Cobá¹,

Sánchez²,

Anderson

et al. 2020

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“…With those fits, Pipe3D provides the total flux, dispersion, and the kinematics of each emission line. The quality of the emission line fits of Pipe3D (and other codes) was tested using MUSE data (Sánchez-Menguiano et al 2018;Bellocchi et al 2019;López-Cobá et al 2020). With the use of the adjacent continuum windows (from the modeled stellar spectra) for each emission line, Pipe3D estimates the stellar continuum flux and provides the equivalent width of each emission line.…”

Section: Stellar Population Analysismentioning

confidence: 99%

SDSS-IV MaNGA: Global and local stellar population properties of elliptical galaxies

Lacerna

Ibarra-Medel

Ávila-Reese

et al. 2020

A&A

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Context. We study the spatially resolved properties of 343 elliptical galaxies with the Mapping Nearby Galaxies at the Apache Point Observatory (MaNGA) survey. Aims. Our goal is to understand the fundamental processes of formation and quenching of elliptical galaxies. Methods. We used the DESI Legacy Imaging Surveys for accurate morphological classification. Based on integrated spectroscopic properties and colors, we classified seven classes of elliptical galaxies. We inferred the stellar age and metallicity gradients out to a 1.5 effective radius (Reff) of classical “red and dead”, recently quenched, and blue star-forming ellipticals (CLEs, RQEs, and BSFs), corresponding to 73%, 10%, and 4% of the sample, respectively. Additionally, we reconstructed their global and radial histories of star formation and mass growth. Results. The mass- and luminosity-weighted age gradients of CLEs are nearly flat or mildly negative, with small differences between both ages. The respective metallicity gradients are negative (∇log[Zmw] = −0.11−0.08+0.07 dex/Reff and ∇log[Zlw] = −0.11−0.07+0.06 dex/Reff, respectively), being flatter as the mass is smaller. The more massive CLEs formed stars earlier and quenched faster than the less massive ones. The CLEs show a weak inside-out growth and a clear inside-out quenching. They finished their quenching globally 3.8 ± 1.2 Gyr ago on average, with quenching time-scales of 3.4 ± 0.8 Gyr. At M⋆ < 1011 M⊙, the age and Z gradients of the RQEs and BSFs are flatter than those of the CLEs, but with larger scatters. They show very weak inside-out growth and quenching, which is slow and not even completed at z ∼ 0 for the BSFs. Instead, the massive RQEs show an outside-in quenching and positive gradients in the luminosity-weighted age and stellar metallicities. The RQEs of all masses quenched 1.2 ± 0.9 Gyr ago on average. Conclusions. Our results for the CLEs are consistent with a two-phase scenario where their inner parts formed by an early and coeval dissipative collapse with a consequent burst of star formation and further quenching, whereas the outer parts continued their assembly, likely by dry mergers. We also discuss some evolutionary scenarios for the RQE and BSF galaxies that would agree with the generic results.

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“…In our case, we assumed a standard 𝑇 = 10 4 𝐾, which is a good approximation for the temperature calculated by López-Sánchez et al (2004) for HCG 31 (𝑇 ∼ 9400 ± 600 𝐾 for the central zone); therefore we used 𝜎 𝑡 ℎ = 9.4 𝑘𝑚𝑠 −1 . For the instrumental width we use the standard 𝜎 𝑖𝑛𝑠𝑡 for MUSE, which has been taken from the literature (Bellocchi et al 2019, 𝜎 𝑖𝑛𝑠𝑡 = 50 𝑘𝑚𝑠 −1 for the H𝛼 wavelength). The uncertainties of 𝜎 𝑜𝑏𝑠 were calculated according to the formula given by Lenz & Ayres (1992) with the fitting parameters of .…”

Section: Kinematics: Radial Velocity and Velocity Dispersionmentioning

confidence: 99%

A MUSE view of the multiple interacting system HCG 31

Gómez-Espinoza

Torres-Flores

Firpo

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present, for the first time, spatially resolved spectroscopy for the entire Hickson Compact Group 31 obtained with the MUSE instrument at the VLT,and an in-depth analysis of this compact group. To obtain a complete understanding of the system, we derived radial velocity and dispersion velocity maps, maps of the ionization mechanism of the system, chemical abundances and their distribution over the whole system, star formation rates and ages of the different star-forming regions, and the spatial distribution of the Wolf-Rayet stellar population. We also reconstructed the star formation history of the galaxies HCG 31 A, C, B and F, measured the emission-line fluxes, and performed a stellar population synthesis. Our main findings are: (i) that there is clearly disturbed kinematics due to the merger event that the system is experiencing; (ii) that the ionization is produced exclusively via star formation except for the nucleus of the galaxy HCG 31 A, where there is a small contribution of shocks; (iii) that there is low oxygen abundance distributed homogeneously through the system; (iv) that there is a prominent population of carbon Wolf-Rayet stars in the central zone of the group; and (v) that there are clear evidences of the tidal origin of the galaxies HCG 31 E, HCG 31 H, and HCG 31 F because they show quite high oxygen abundances for their stellar mass. All these findings are clear evidence that HCG 31 is currently in an early merging phase and manifesting a starburst in its central region.

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

Cited by 6 publications

References 68 publications

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

SDSS-IV MaNGA: Global and local stellar population properties of elliptical galaxies

A MUSE view of the multiple interacting system HCG 31

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