Tracing the outer disk of NGC 300: An ultraviolet view

Mondal, Chayan; Subramaniam, Annapurni; George, Koshy

doi:10.1007/s12036-019-9603-4

Cited by 6 publications

(5 citation statements)

References 43 publications

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“…This scale length is consistent with those measured in previous optical and IR studies (Gogarten et al 2010;Jang et al 2020). The UV disk of NGC 300 is known to be more extended than the optical/IR disk (∼2.7 kpc in the near-UV, hereafter NUV, see Mondal et al 2019). For comparison, we also show the Galaxy Evolution Explorer (GALEX) NUV surface brightness profile in Figure 1, for which we measure a scale length of ∼2.4 kpc (see Section 2.1.5 for a discussion of GALEX data.)…”

Section: Spitzer Irac and Mipssupporting

confidence: 90%

“…The galaxy has been observed across nearly the entire electromagnetic spectrum, and exhibits a metallicity gradient with metallicity decreasing by ∼0.08Z e kpc -1 (Gogarten et al 2010; Kudritzki et al 2008). The SFR of NGC 300 is generally reported to be ∼0.08 − 0.46 M e yr −1 by different tracers, such as the Hubble Space Telescope (HST) resolved stellar populations (Gogarten et al 2010), UV observations (Mondal et al 2019), Hα emission (Karachentsev & Kaisina 2013), and mid-IR observations (Helou et al 2004). NGC 300 contains an ultraluminous X-ray source (ULX; e.g., see review by Binder et al 2020 and references therein) and the luminous Wolf-Rayet + BH binary NGC 300 X-1 (Binder et al 2021), although the majority of XRBs in the galaxy are of lower luminosity (∼10 36-37 erg s −1 ; Binder et al 2012Binder et al , 2017, and the specific SFR of NGC 300 suggests that its XRB population is likely a mix of HMXBs and LMXBs (Lehmer et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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A Panchromatic Study of the X-Ray Binary Population in NGC 300 on Subgalactic Scales

Binder,

Williams,

Payne

et al. 2024

ApJ

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The population-wide properties and demographics of extragalactic X-ray binaries (XRBs) correlate with the star formation rates (SFRs), stellar masses (M ⋆), and environmental factors (such as metallicity, Z) of their host galaxy. Although there is evidence that XRB scaling relations (L X/SFR for high-mass XRBs (HMXBs) and L X/M ⋆ for low-mass XRBs) may depend on metallicity and stellar age across large samples of XRB-hosting galaxies, disentangling the effects of metallicity and stellar age from stochastic effects, particularly on subgalactic scales, remains a challenge. We use archival X-ray through IR observations of the nearby galaxy NGC 300 to self-consistently model the broadband spectral energy distribution and examine radial trends in its XRB population. We measure a current (<100 Myr) SFR of 0.18 ± 0.08 M⊙ yr−1 and stellar mass M ⋆ = ( 2.15 − 0.14 + 0.26 ) × 10 9 M⊙. Although we measure a metallicity gradient and radially resolved star formation histories that are consistent with the literature, there is a clear excess in the number of X-ray sources below ∼1037 erg s−1 that are likely a mix of variable XRBs and additional background active galactic nuclei. When we compare the subgalactic L X/SFR ratios as a function of Z to the galaxy-integrated L X-SFR-Z relationships from the literature, we find that only the regions hosting the youngest (≲30 Myr) HMXBs agree with predictions, hinting at time evolution of the L X–SFR–Z relationship.

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Section: Spitzer Irac and Mipssupporting

confidence: 90%

Section: Introductionmentioning

confidence: 99%

A Panchromatic Study of the X-Ray Binary Population in NGC 300 on Subgalactic Scales

Binder,

Williams,

Payne

et al. 2024

ApJ

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“…They showed that the disparity between the H and other warp tracers is significant in both phase and amplitude, while the Cepheids appear to mirror the H warp, implying that they formed in-situ in the warp. Evidence of star formation in the outskirts of galactic discs has also been inferred in external galaxies via UV-bright stellar complexes (Thilker et al 2005;Zaritsky & Christlein 2007;Herbert-Fort et al 2010;Mondal et al 2019). These stellar complexes are observed far outside the optical discs, which are usually warped, and in one case (Thilker et al 2005) they were directly associated with the warped H disc.…”

Section: Introductionmentioning

confidence: 95%

How stars formed in warps settle into (and contaminate) thick discs

Khachaturyants,

Silva,

Debattista

2021

Preprint

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In recent years star formation has been discovered in the Milky Way's warp. These stars formed in the warp (warp stars) must eventually settle into the plane of the disc. We use an 𝑁-body+smooth particle hydrodynamics model of a warped galaxy to study how warp stars settle into the disc. By following warp stars in angular momentum space, we show that they first tilt to partially align with the main disc in a time scale of ∼ 1 Gyr. Then, once differential precession halts this process, they phase mix into an axisymmetric distribution on a time scale of ∼ 6 Gyr. The warp stars end up contaminating the geometric thick disc. Because the warp in our fiducial simulation is growing, the warp stars settle to a distribution with a negative vertical age gradient as younger stars settle further from the mid-plane. While vertically extended, warp star orbits are still nearly circular and they are therefore subject to radial migration, with a net movement inwards. As a result warp stars can be found throughout the disc. The density distribution of a given population of warp stars evolves from a torus to an increasingly centrally filled-in density distribution. Therefore we argue that, in the Milky Way, warp stars should be found in the Solar Neighbourhood. Moreover, settled warp stars may constitute part of the young flaring population seen in the Milky Way's outskirts.

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“…They showed that the disparity between the Hi and other warp tracers is significant in both phase and amplitude, while the Cepheids appear to mirror the Hi warp, implying that they formed in-situ in the warp. Evidence of star formation in the outskirts of galactic discs has also been inferred in external galaxies via UV-bright stellar complexes (Thilker et al 2005;Zaritsky & Christlein 2007;Herbert-Fort et al 2010;Mondal et al 2019). These stellar complexes are observed far outside the optical discs, which are usually warped, and in one case (Thilker et al 2005) they were directly associated with the warped Hi disc.…”

mentioning

confidence: 95%

How stars formed in warps settle into (and contaminate) thick discs

Khachaturyants

Silva

Debattista

2021

Monthly Notices of the Royal Astronomical Society

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In recent years star formation has been discovered in the Milky Way’s warp. These stars formed in the warp (warp stars) must eventually settle into the plane of the disc. We use an N-body+smooth particle hydrodynamics model of a warped galaxy to study how warp stars settle into the disc. By following warp stars in angular momentum space, we show that they first tilt to partially align with the main disc in a time scale of $\sim 1 {\:{\rm Gyr}}$. Then, once differential precession halts this process, they phase mix into an axisymmetric distribution on a time scale of $\sim 6 {\:{\rm Gyr}}$. The warp stars end up contaminating the geometric thick disc. Because the warp in our fiducial simulation is growing, the warp stars settle to a distribution with a negative vertical age gradient as younger stars settle further from the mid-plane. While vertically extended, warp star orbits are still nearly circular and they are therefore subject to radial migration, with a net movement inwards. As a result warp stars can be found throughout the disc. The density distribution of a given population of warp stars evolves from a torus to an increasingly centrally filled-in density distribution. Therefore we argue that, in the Milky Way, warp stars should be found in the Solar Neighbourhood. Moreover, settled warp stars may constitute part of the young flaring population seen in the Milky Way’s outskirts.

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Tracing the outer disk of NGC 300: An ultraviolet view

Cited by 6 publications

References 43 publications

A Panchromatic Study of the X-Ray Binary Population in NGC 300 on Subgalactic Scales

A Panchromatic Study of the X-Ray Binary Population in NGC 300 on Subgalactic Scales

How stars formed in warps settle into (and contaminate) thick discs

How stars formed in warps settle into (and contaminate) thick discs

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