The Impact of Star Formation Histories on Stellar Mass Estimation: Implications from the Local Group Dwarf Galaxies

Zhang, Hong Xin; Puzia, Thomas H.; Weisz, Daniel R.

doi:10.3847/1538-4365/aa937b

Cited by 51 publications

(52 citation statements)

References 130 publications

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“…The former method typically relies on some sort of theoretical or empirical underpinning relating observed quantities to physical properties, which can introduce some level of uncertainty. For example, uncertainties in galaxy star formation histories, stellar evolution tracks, obscuring dust geometries, and the initial mass function propagate to uncertainties in derived SFRs and stellar masses of observed galaxies (e.g., Maraston et al 2006;Conroy et al 2009;Michałowski et al 2010;Dunlop 2011;Walcher et al 2011;Conroy 2013;Leja et al 2017Leja et al , 2019Zhang et al 2017;Lower et al 2020). Similarly, uncertainties in spectral energy distribution (SED) modeling, or the conversion between emission-line strengths, continuum strengths, and gas masses are present in any measurement of the ISM properties of galaxies (e.g., Feldmann et al 2011;Narayanan et al 2011bCasey 2012;Bolatto et al 2013;Scoville et al 2014;Liang et al 2018;Privon et al 2018).…”

Section: Introductionmentioning

confidence: 99%

powderday: Dust Radiative Transfer for Galaxy Simulations

Narayanan

Turk

Robitaille³

et al. 2021

ApJS

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We present POWDERDAY (available at https://github.com/dnarayanan/powderday), a flexible, fast, open-source dust radiative transfer package designed to interface with both idealized and cosmological galaxy formation simulations. POWDERDAY builds on FSPS stellar population synthesis models, and HYPERION dust radiative transfer, and employs YT to interface between different software packages. We include our stellar population synthesis modeling on the fly, allowing significant flexibility in the assumed stellar physics and nebular line emission. The dust content follows either simple observationally motivated prescriptions (i.e., constant dust-tometals ratios, or dust-to-gas ratios that vary with metallicity), direct modeling from galaxy formation simulations that include dust physics, as well as a novel approach that includes the dust content via learning-based algorithms from the SIMBA cosmological galaxy formation simulation. Active galactic nuclei (AGNs) can additionally be included via a range of prescriptions. The output of these models are broadband (912 Å-1 mm) spectral energy distributions (SEDs), as well as filter-convolved monochromatic images. POWDERDAY is designed to eliminate last-mile efforts by researchers that employ different hydrodynamic galaxy formation models and seamlessly interfaces with GIZMO, AREPO, GASOLINE, CHANGA, and ENZO. We demonstrate the capabilities of the code via three applications: a model for the star formation rate-infrared luminosity relation in galaxies (including the impact of AGNs), the impact of circumstellar dust around AGB stars on the mid-infrared emission from galaxy SEDs, and the impact of galaxy inclination angle on dust attenuation laws.

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Section: Introductionmentioning

confidence: 99%

powderday: Dust Radiative Transfer for Galaxy Simulations

Narayanan

Turk

Robitaille³

et al. 2021

ApJS

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“…Errors on colour/luminosity measurements are propagated separately. For the mass range of most galaxies in PROBES, the Roediger & Courteau (2015) mass-tolight transformations are consistent with other transformations such as Zhang et al (2017). Numerous uncertainty factors affect stellar mass estimates and are described in the luminosity and colour sections (Sections 3.3.2 and 3.3.4) Equation 10 expresses the stellar mass calculation.…”

Section: * [M ]mentioning

confidence: 62%

“…We choose g − z colour over g − r (which can also be measured from the DESI-LIS) for its longer baseline and low measurement error. Colours are useful as inputs to colour mass-to-light transformations (Taylor et al 2011;Conroy 2013;Roediger & Courteau 2015;Zhang et al 2017;García-Benito et al 2019) and can be used to construct scaling relations on their own. The g − z colours are calculated as:…”

Section: G − Z [Mag]mentioning

confidence: 99%

The Intrinsic Scatter of Galaxy Scaling Relations

Stone,

Courteau,

Arora

2021

Preprint

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We present a compendium of disk galaxy scaling relations and a detailed characterization of their intrinsic scatter. Observed scaling relations are typically characterized by their slope, intercept, and scatter; however, these parameters are a mixture of observational errors and astrophysical processes. We introduce a novel Bayesian framework for computing the intrinsic scatter of scaling relations that accounts for nonlinear error propagation and covariant uncertainties. Bayesian intrinsic scatters are ∼ 25 percent more accurate than those obtained with a first-order classical method, which systematically underestimates the true intrinsic scatter. Structural galaxy scaling relations based on velocity (V 23.5 ), size (R 23.5 ), luminosity (L 23.5 ), colour (g − z), central stellar surface density (Σ 1 ), stellar mass (M * ), dynamical mass (M dyn ), stellar angular momentum (j * ), and dynamical angular momentum (j dyn ), are examined to demonstrate the power and importance of the Bayesian formalism. Our analysis is based on a diverse selection of over 1000 late-type galaxies from the Photometry and Rotation Curve Observations from Extragalactic Surveys compilation with deep optical photometry and extended rotation curves. We determine the tightest relation for each parameter by intrinsic orthogonal scatter, finding M * − V 23.5 , R 23.5 − j * , and L 23.5 − j dyn to be especially tight. The scatter of the R 23.5 − L 23.5 , V 23.5 − (g − z), and R 23.5 − j dyn relations is mostly intrinsic, making them ideal for galaxy formation and evolutionary studies. Our code to compute the Bayesian intrinsic scatter of any scaling relation is also presented. We quantify the correlated nature of many uncertainties in galaxy scaling relations and scrutinize the uncertain nature of disk inclination corrections and their effect on scatter estimates.

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“…Indeed, galaxy star-formation histories are complex. However, it is shown that scatter in the mass-to-light ratio derived from different starformation history for a given color is ∼0.2 dex, see §4.3 Zhang et al (2017). Therefore, we consider ±0.2 dex as a typical conservative error on our stellar mass estimates.…”

Section: Data Analysis 31 Analysis Of Archival Datamentioning

confidence: 94%

MCG+07-20-052: Interacting Dwarf Pair in a Group Environment

Paudel

Sengupta

Yoon³

et al. 2020

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We present an observational study of the interacting pair of dwarf galaxies, MCG+07-20-052 , in the vicinity of Milky Way mass spiral galaxy NGC 2998. MCG+07-20-052 is located at a sky-projected distance of 105 kpc from NGC 2998 and the two have a relative line-of-sight velocity of 60 km s −1 . We observed tidal tail-like extensions on both members (D1 and D2) of the interacting pair MCG+07-20-052 . The interacting dwarf galaxies, D1 and D2, have B-band absolute magnitudes of −17.17 and −17.14 mag, respectively, and D2 is significantly bluer than D1. We obtained HI 21 cm line data of the NGC 2998 system using the Giant Metrewave Radio Telescope (GMRT) to get a more detailed view of the neutral hydrogen (HI) emission in the interacting dwarf galaxies and in the galaxy members of the NGC 2998 group. Evidence of a merger between the dwarf galaxies in the MCG+07-20-052 is also present in the HI kinematics and morphology where we find that the HI is mostly concentrated around D2, which also shows a higher level of star-forming activity and bluer g − r color index compared to D1. In addition, we detect extended tenuous HI emission around another member galaxy, NGC 3006, located close to the MCG+07-20-052 -pair at a sky-projected distance of 41 kpc. We compare here our results from the MCG+07-20-052 pair-NGC 2998 system with other known LMC-SMC-Milky Way type systems and discuss the possible origin of the dwarf-dwarf interaction.

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The Impact of Star Formation Histories on Stellar Mass Estimation: Implications from the Local Group Dwarf Galaxies

Cited by 51 publications

References 130 publications

powderday: Dust Radiative Transfer for Galaxy Simulations

powderday: Dust Radiative Transfer for Galaxy Simulations

The Intrinsic Scatter of Galaxy Scaling Relations

MCG+07-20-052: Interacting Dwarf Pair in a Group Environment

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