A study of the ionized gas in Stephan's Quintet from integral field spectroscopy observations★

Rodríguez-Baras, M.; Rosales-Ortega, F. F.; Díaz, Ángeles I.; Sánchez, S. F.; Pasquali, A.

doi:10.1093/mnras/stu851

Cited by 12 publications

(27 citation statements)

References 53 publications

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“…All the properties studied in Fig. 15 are consistent with the presence of an inner-outer variation along the NI tails in the line of the results obtained by Iglesias-Páramo et al (2012) and Rodríguez-Baras et al (2014). Finally, the relation between log(N/O) and 12+log(O/H) for the SQ HII region is presented in Fig.…”

Section: Discussion and Summarysupporting

confidence: 86%

Searching for intergalactic star forming regions in Stephan’s Quintet with SITELLE

Puertas

Vı́lchez

Iglésias-Páramo

et al. 2021

A&A

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Based on SITELLE spectroscopy data, we studied the ionised gas emission for the 175 Hα emission regions in the Stephan's Quintet (SQ). In this paper we perform a detailed analysis of the star formation rate (SFR), oxygen abundance, and nitrogen-to-oxygen abundance ratio (N/O) of the SQ regions, with the intention of exploring the provenance and evolution of this complex structure. According to the BPT diagram, we found 91 HII, 17 composite, and 7 active galactic nucleus-like regions in SQ. Several regions are compatible with fast shocks models without a precursor for solar metallicity and low density (n = 0.1 cm −3), with velocities in the range of 175-300 km s −1. We derived the total SFR in SQ (log(SFR/M yr −1 =0.496). Twenty-eight percent of the total SFR in SQ comes from starburst A, while 9% is in starburst B, and 45% comes from the regions with a radial velocity lower than 6160 km s −1. For this reason, we assume that the material prior to the collision with the new intruder does not show a high SFR, and therefore SQ was apparently quenched. When considering the integrated SFR for the whole SQ and the new intruder, we found that both zones have a SFR consistent with those obtained in the SDSS star-forming galaxies. At least two chemically different gas components cohabit in SQ where, on average, the regions with high radial velocities (v>6160 km s −1) have lower values of oxygen abundance and N/O than those with low radial velocities (v≤6160 km s −1). The values found for the line ratios considered in this study, as well as in the oxygen abundance and N/O for the southern debris region and the northernmost tidal tail, are compatible with regions belonging to the outer part of the galaxies. We highlight the presence of inner-outer variation for metallicity and some emission line ratios along the new intruder strands and the young tidal tail south strand. Finally, the SQ Hα regions are outside the galaxies because the interactions have dispersed the gas to the peripheral zones.

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Section: Discussion and Summarysupporting

confidence: 86%

Searching for intergalactic star forming regions in Stephan’s Quintet with SITELLE

Puertas

Vı́lchez

Iglésias-Páramo

et al. 2021

A&A

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“…This multiplicity of velocity components (also confirmed with optical spectroscopy of the faint ionized gas by Iglesias-Páramo et al 2012; Konstantopoulos et al 2014;Rodríguez-Baras et al 2014) implies a complex interplay between the intruder galaxy's gas and the pre-and post-shocked gas lying in the group. Unfortunately, although we expect the warm H 2 emission discussed in the current paper to primarily be post-shocked gas, we do not have the velocity resolution to make a detailed comparison with the previously published spectroscopy.…”

Section: Introductionmentioning

confidence: 54%

“…The filament, which lies between NGC 7319 and NGC 7318b, was first observed in radio continuum emission and later in X-rays. Observations strongly suggest that the gas in the filament is heated by shocks driven into the intergroup medium by the "intruder" galaxy NGC 7318b (Gao & Xu 2000;Xu et al 2003Xu et al , 2005O'Sullivan et al 2009;Iglesias-Páramo et al 2012;Konstantopoulos et al 2014;Rodríguez-Baras et al 2014). The galaxy is likely colliding from behind the group with a blueshifted radial velocity of 800-1000 km s −1 with respect to the majority of the gas in the group.…”

Section: Introductionmentioning

confidence: 99%

Powerful H₂ Line Cooling in Stephan’s Quintet. II. Group-wide Gas and Shock Modeling of the Warm H₂ and a Comparison with [C ii] 157.7 μm Emission and Kinematics

Appleton

Guillard

Togi

et al. 2017

ApJ

106

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We map for the first time the two-dimensional H 2 excitation of warm intergalactic gas in Stephanʼs Quintet on group-wide (50×35 kpc 2 ) scales to quantify the temperature, mass, and warm H 2 mass fraction as a function of position using Spitzer. Molecular gas temperatures are seen to rise (to T > 700 K) and the slope of the power-law density-temperature relation flattens along the main ridge of the filament, defining the region of maximum heating. We also performed MHD modeling of the excitation properties of the warm gas, to map the velocity structure and energy deposition rate of slow and fast molecular shocks. Slow magnetic shocks were required to explain the power radiated from the lowest-lying rotational states of H 2 , and strongly support the idea that energy cascades down to small scales and low velocities from the fast collision of NGC 7318b with group-wide gas. The highest levels of heating of the warm H 2 are strongly correlated with the large-scale stirring of the medium as measured by [C II] spectroscopy with Herschel. H 2 is also seen associated with a separate bridge that extends toward the Seyfert nucleus in NGC 7319, from both Spitzer and CARMA CO observations. This opens up the possibility that both galaxy collisions and outflows from active galactic nuclei can turbulently heat gas on large scales in compact groups. The observations provide a laboratory for studying the effects of turbulent energy dissipation on groupwide scales, which may provide clues about the heating and cooling of gas at high z in early galaxy and protogalaxy formation.

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“…However, if we take into account the errors in the measurements, in the latter case the slope of the outer gradient is also compatible with zero, although because of the low number of H II regions in the outer zone, we are not able to give a conclusion. The flattening in the oxygen gradients in the outer part was also found for individual galaxies (Martin & Roy 1995;Bresolin et al 2009b;Goddard et al 2011;Rosales et al 2011;Zahid & Bresolin 2011;Bresolin et al 2012;Marino et al 2012;Torres-Flores et al 2014;Rodríguez-Baras et al 2014;Miralles-Caballero et al 2014), a small sample of interacting galaxies (Werk et al 2011), a large sample of objects (Sánchez et al 2012(Sánchez et al , 2014, and even for the Milky Way (Esteban et al 2013). Basically, there are four theoretical scenarios to explain the flattening of the oxygen abundance gradients at a given galactocentric distance:…”

Section: Discussionmentioning

confidence: 85%

Interaction effects on galaxy pairs with Gemini/GMOS – II: oxygen abundance gradients

Rosa¹,

Dors²,

Krabbe³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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In this paper, we derive oxygen abundance gradients from H II regions located in 11 galaxies in eight systems of close pairs. Long-slit spectra in the range 4400-7300 Å were obtained with the Gemini Multi-Object Spectrograph at Gemini South (GMOS-S). Spatial profiles of oxygen abundance in the gaseous phase along galaxy discs were obtained using calibrations based on strong emission lines (N2 and O3N2). We found oxygen gradients to be significantly flatter for all the studied galaxies than those in typical isolated spiral galaxies. Four objects in our sample, AM 1219A, AM 1256B, AM 2030A and AM 2030B, show a clear break in the oxygen abundance at galactocentric radius R/R 25 between 0.2 and 0.5. For AM 1219A and AM 1256B, we found negative slopes for the inner gradients, and for AM 2030B, we found a positive slope. All three cases show a flatter behaviour to the outskirts of the galaxies. For AM 2030A, we found a positive slope for the outer gradient, while the inner gradient is almost compatible with a flat behaviour. We found a decrease of star formation efficiency in the zone that corresponds to the oxygen abundance gradient break for AM 1219A and AM 2030B. For the former, a minimum in the estimated metallicities was found very close to the break zone, which could be associated with a corotation radius. However, AM 1256B and AM 2030A, present a star formation rate maximum but not an extreme oxygen abundance value. All four interacting systems that show oxygen gradient breaks have extreme SFR values located very close to break zones.The H II regions located in close pairs of galaxies follow the same relation between the ionization parameter and the oxygen abundance as those regions in isolated galaxies.

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A study of the ionized gas in Stephan's Quintet from integral field spectroscopy observations★

Cited by 12 publications

References 53 publications

Searching for intergalactic star forming regions in Stephan’s Quintet with SITELLE

Searching for intergalactic star forming regions in Stephan’s Quintet with SITELLE

Powerful H₂ Line Cooling in Stephan’s Quintet. II. Group-wide Gas and Shock Modeling of the Warm H₂ and a Comparison with [C ii] 157.7 μm Emission and Kinematics

Interaction effects on galaxy pairs with Gemini/GMOS – II: oxygen abundance gradients

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A study of the ionized gas in Stephan's Quintet from integral field spectroscopy observations★

Cited by 12 publications

References 53 publications

Searching for intergalactic star forming regions in Stephan’s Quintet with SITELLE

Searching for intergalactic star forming regions in Stephan’s Quintet with SITELLE

Powerful H2 Line Cooling in Stephan’s Quintet. II. Group-wide Gas and Shock Modeling of the Warm H2 and a Comparison with [C ii] 157.7 μm Emission and Kinematics

Interaction effects on galaxy pairs with Gemini/GMOS – II: oxygen abundance gradients

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Product

Resources

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Powerful H₂ Line Cooling in Stephan’s Quintet. II. Group-wide Gas and Shock Modeling of the Warm H₂ and a Comparison with [C ii] 157.7 μm Emission and Kinematics