The Extended Baryonic Halo of NGC 3923

Miller, Bryan W.; Ahumada, Tomás; Puzia, Thomas H.; Candlish, Graeme N.; McGaugh, Stacy S.; Mihos, J. Christopher; Sanderson, Robyn E.; Schirmer, M.; Smith, Rory; Taylor, Matthew A.

doi:10.3390/galaxies5030029

Cited by 4 publications

(5 citation statements)

References 25 publications

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“…Figure 14 shows that both subpopulations do not seem to have reached a background level within our GMOS mosaic. The slope found for the red GCs is similar to that reported for other massive early-type galaxies ( ever, the blue GC candidates present a shallower slope, similar to that found for NGC 3923 (Faifer et al 2011;Miller et al 2017). Interestingly, this is a massive elliptical shell galaxy as well, located in a poor group of galaxies.…”

Section: Spatial Distributionsupporting

confidence: 87%

“…ever, the blue GC candidates present a shallower slope, similar to that found for NGC 3923 (Faifer et al 2011;Miller et al 2017). Interestingly, this is a massive elliptical shell galaxy as well, located in a poor group of galaxies.…”

Section: Spatial Distributionsupporting

confidence: 77%

“…As shown in Section 5.2, the GC system of NGC 1395, in particular the blue subpopulation, shows a shallower slope of the density profile compared to other GC systems belonging to massive E galaxies (see e.g., Faifer et al 2011). In recent years, using wide-field imaging, different authors have found that some GC systems belonging to massive galaxies extend to large galactocentric radii ( 100 kpc; Kartha et al 2016;Miller et al 2017;Taylor et al 2017). In this context, we decided to extend the integration of the density profile to a maximum galactocentric radius of 165 kpc.…”

Section: Luminosity Function and Total Gc Populationmentioning

confidence: 94%

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Tracing the assembly history of NGC 1395 through its Globular Cluster System

Escudero

Faifer

Castelli

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We used deep Gemini-South/GMOS g ′ r ′ i ′ z ′ images to study the globular cluster (GC) system of the massive elliptical galaxy NGC 1395, located in the Eridanus supergroup. The photometric analysis of the GC candidates reveals a clear colour bimodality distribution, indicating the presence of "blue" and "red" GC subpopulations. While a negative radial colour gradient is detected in the projected spatial distribution of the red GCs, the blue GCs display a shallow colour gradient. The blue GCs also display a remarkable shallow and extended surface density profile, suggesting a significant accretion of low-mass satellites in the outer halo of the galaxy. In addition, the slope of the projected spatial distribution of the blue GCs in the outer regions of the galaxy, is similar to that of the X-ray halo emission. Integrating up to 165 kpc the profile of the projected spatial distribution of the GCs, we estimated a total GC population and specific frequency of 6000±1100 and S N =7.4±1.4, respectively. Regarding NGC 1395 itself, the analysis of the deep Gemini/GMOS images shows a low surface brightness umbrella-like structure indicating, at least, one recent merger event. Through relations recently published in the literature, we obtained global parameters, such as M stellar = 9.32 × 10 11 M⊙ and M h = 6.46 × 10 13 M⊙. Using public spectroscopic data, we derive stellar population parameters of the central region of the galaxy by the full spectral fitting technique. We have found that, this region, seems to be dominated for an old stellar population, in contrast to findings of young stellar populations from the literature.

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Section: Spatial Distributionsupporting

confidence: 87%

Section: Spatial Distributionsupporting

confidence: 77%

Section: Luminosity Function and Total Gc Populationmentioning

confidence: 94%

See 1 more Smart Citation

Tracing the assembly history of NGC 1395 through its Globular Cluster System

Escudero

Faifer

Castelli

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…There can be just one shell in a galaxy, but also up to a few dozen (Prieur 1988;Bílek et al 2016Bílek et al , 2020Miller et al 2017). Shells can be aligned with the major axis of the host galaxy or be distributed randomly in azimuth (Wilkinson et al 1987;Prieur 1990).…”

Section: Introductionmentioning

confidence: 99%

Origin of the spectacular tidal shells of galaxy NGC 474

Bílek

Fensch

Ebrová

et al. 2022

A&A

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Context. The lenticular galaxy NGC 474 hosts a rich system of tidal shells and streams, some of which are exceptionally bright. Two teams recently presented spectroscopic observations of the brightest shells. These were the first shell spectra ever observed in integrated starlight. The authors studied the stellar populations of the shell, of the center of the galaxy, and of its globular clusters. The precise formation scenario for the tidal features of this prominent galaxy still remained unclear, however. Aims. Here, we add further clues on their formation from the radii of the shells, and we present a scenario for the formation of the tidal features that seems to be unique and can explain all available data. Methods. Shell radii were analyzed with the shell identification method, and we ran self-consistent simulations of the formation of the tidal features. We considered Newtonian as well as MOND gravity. Results. Observations suggest that the tidal features originate from the accretion of a spiral galaxy. According to the shell identification method, the merging galaxies first collided 1.3 Gyr ago and then again 0.9 Gyr ago, thereby forming the shells in two generations. This would also explain the young ages of stellar populations in the center of the galaxy and the young age of the globular clusters. The analytic models of shell propagation that underlie the shell identification method are verified by a simulation. The simulations reproduce the observed morphology of the tidal features well. The accreted spiral likely reached NGC 474 on the plane of the sky nearly radially from the south, its rotation axis pointing toward us. It probably had a stellar mass of about one-sixth of NGC 474, that is, 109.8 M⊙. Apparently, all tidal features in the galaxy originate from one merger.

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“…There can be only one shell in a galaxy but also up to a few tens of them (Prieur 1988;Bílek et al 2016;Miller et al 2017;Bílek et al 2020). Shells can be aligned with the major axis of the host galaxy or distributed randomly in azimuth (Wilkinson et al 1987;Prieur 1990).…”

Section: Introductionmentioning

confidence: 99%

Origin of the spectacular tidal shells of galaxy NGC474

Bílek,

Fensch,

Ebrová

et al. 2021

Preprint

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Context. The lenticular galaxy NGC 474 hosts a rich system of tidal shells and streams, some of which are exceptionally bright. Two teams recently presented spectroscopic observations of the brightest shells. These were the first shell spectra ever observed in integrated starlight. The authors studied the stellar populations of the shell, of the center of the galaxy and of its globular clusters. The precise formation scenario for the tidal features of this prominent galaxy however still remained unclear.Aims. Here, we add further clues on their formation from the radii of the shells, and we present a scenario for the formation of the tidal features that seems to be unique and explaining all available data. Methods. Shell radii are analyzed with the shell identification method, and we run self-consistent simulations of the formation of the tidal features. We consider Newtonian as well as MOND gravity. Results. Observations suggest that the tidal features originate from the accretion of a spiral galaxy. The shell identification method yields that the merging galaxies collided first 1.3 Gyr ago and then again 0.9 Gyr ago, thereby forming the shells in two generations. This would also explain the young ages of stellar populations in the center of the galaxy and the young age of the globular clusters. The analytic models of shell propagation, that underlie the shell identification method, are verified by a simulation. The simulations reproduce well the observed morphology of the tidal features. The accreted spiral likely reached NGC 474 nearly radially, in the plane of the sky, from the south, its rotation axis pointing toward us. It should have had a stellar mass of around 1/6 of NGC 474, i.e. 10 9.8 M . It seems that all tidal features in the galaxy originate from one merger.

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The Extended Baryonic Halo of NGC 3923

Cited by 4 publications

References 25 publications

Tracing the assembly history of NGC 1395 through its Globular Cluster System

Tracing the assembly history of NGC 1395 through its Globular Cluster System

Origin of the spectacular tidal shells of galaxy NGC 474

Origin of the spectacular tidal shells of galaxy NGC474

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