The Distance to M51*

McQuinn, Kristen B. W.; Skillman, Evan D.; Dolphin, Andrew E.; Berg, Danielle A.; Kennicutt, Robert C.

doi:10.3847/0004-637x/826/1/21

Cited by 80 publications

(50 citation statements)

References 73 publications

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“…An interesting comparison can be found in Leo P, a nearby (D=1.62±0.15 Mpc; McQuinn et al 2015b), extremely low-mass (log(M H I )=8.1 × 10 5 M e ) galaxy that was discovered by ALFALFA Rhode et al 2013). In a detailed H I study by Bernstein-Cooper et al (2014), the authors examine deep VLA H I 21 cm data that are very similar to the data presented here for the SHIELD galaxies.…”

Section: Discussionmentioning

confidence: 85%

Shield: Neutral Gas Kinematics and Dynamics

McNichols

Teich

Nims³

et al. 2016

ApJ

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We present kinematic analyses of the 12 galaxies in the "Survey of H I in Extremely Low-mass Dwarfs" (SHIELD). We use multi-configuration interferometric observations of the H I 21 cm emission line from the Karl G. Jansky Very Large Array (VLA) 22 to produce image cubes at a variety of spatial and spectral resolutions. Both two-and three-dimensional fitting techniques are employed in an attempt to derive inclination-corrected rotation curves for each galaxy. In most cases, the comparable magnitudes of velocity dispersion and projected rotation result in degeneracies that prohibit unambiguous circular velocity solutions. We thus make spatially resolved position-velocity cuts, corrected for inclination using the stellar components, to estimate the circular rotation velocities. We find v circ  30 km s −1 for the entire survey population. Baryonic masses are calculated using singledish H I fluxes from Arecibo and stellar masses derived from HST and Spitzer imaging. Comparison is made with total dynamical masses estimated from the position-velocity analysis. The SHIELD galaxies are then placed on the baryonic Tully-Fisher relation. There exists an empirical threshold rotational velocity, Vrot < 15 km s −1 , below which current observations cannot differentiate coherent rotation from pressure support. The SHIELD galaxies are representative of an important population of galaxies whose properties cannot be described by current models of rotationally dominated galaxy dynamics.

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Section: Discussionmentioning

confidence: 85%

Shield: Neutral Gas Kinematics and Dynamics

McNichols

Teich

Nims³

et al. 2016

ApJ

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“…are outflows a necessary requirement for super-orbital modulation in the X-ray light-curves of PULXs? A particularly interesting system is M51 ULX-7, a known ULX system located in the Whirlpool galaxy at a distance of (8.58±0.1) Mpc (McQuinn et al 2016). The detection of coherent pulsations (P ∼ 2.8 s) and an orbital period of ∼ 2 d confirm the system as a new PULX (Rodríguez Castillo et al 2019).…”

Section: Introductionmentioning

confidence: 98%

M51 ULX-7: superorbital periodicity and constraints on the neutron star magnetic field

Vasilopoulos

Lander

Koliopanos

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In the current work we explore the applicability of standard theoretical models of accretion to the observed properties of M51 ULX-7. The spin-up rate and observed X-ray luminosity are evidence of a neutron star with a surface magnetic field of 2 − 7 × 10 13 G, rotating near equilibrium. Analysis of the X-ray light-curve of the system (Swift/XRT data) reveals the presence of a ∼39 d super-orbital period. We argue that the super-orbital periodicity is due to disc precession, and that material is accreted onto the neutron star at a constant rate throughout it. Moreover, by attributing this modulation to the free precession of the neutron star we estimate a surface magnetic field strength of 3 − 4 × 10 13 G. The agreement of these two independent estimates provide strong constraints on the surface polar magnetic field strength of the neutron star.

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“…Bayesian maximum likelihood techniques have also been used to measure TRGB luminosities and can result in lower statistical uncertainties of theorder of0.1 mag or less (e.g., Makarov et al 2006;Conn et al 2012;McQuinn et al 2016). For our purposes of identifying the TRGB in order to separate the RGB and AGB populations, the use of an edgedetection filter provides sufficient precision of 0.2 mag.…”

Section: Identifying the Trgbmentioning

confidence: 99%

DUSTiNGS. III. DISTRIBUTION OF INTERMEDIATE-AGE AND OLD STELLAR POPULATIONS IN DISKS AND OUTER EXTREMITIES OF DWARF GALAXIES

McQuinn

Boyer

Mitchell

et al. 2017

ApJ

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We have traced the spatial distributions of intermediate-age and old stars in nine dwarf galaxies in the distant parts of the Local Group, using multi-epoch 3.6 and 4.5 μm data from the DUST in Nearby Galaxies with Spitzer (DUSTiNGS) survey. Using complementary optical imaging from the Hubble Space Telescope, we identify the tip of the red giant branch (TRGB) in the 3.6 μm photometry, separating thermally pulsating asymptotic giant branch stars from the larger red giant branch populations. Unlike the constant TRGB in the I band, at 3.6 μm,the TRGB magnitude varies by ∼0.7 mag, making it unreliable as a distance indicator. The intermediate-age and old stars are well mixed in two-thirds of the sample, with no evidence of a gradient in the ratio of the intermediate-age to old stellar populations outside the central ∼1′-2′. Variable AGB stars are detected in the outer extremities of the galaxies, indicating that chemical enrichment from these dust-producing stars may occur in the outer regions of galaxies with some frequency. Theories of structure formation in dwarf galaxies must account for the lack of radial gradients in intermediate-age populations and the presence of these stars in the outer extremities of dwarfs. Finally, we identify unique features in individual galaxies, such as extended tidal features in SexA and SagDIG and a central concentration of AGB stars in the inner regions of NGC185 and NGC147.

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The Distance to M51*

Cited by 80 publications

References 73 publications

Shield: Neutral Gas Kinematics and Dynamics

Shield: Neutral Gas Kinematics and Dynamics

M51 ULX-7: superorbital periodicity and constraints on the neutron star magnetic field

DUSTiNGS. III. DISTRIBUTION OF INTERMEDIATE-AGE AND OLD STELLAR POPULATIONS IN DISKS AND OUTER EXTREMITIES OF DWARF GALAXIES

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