The Planetary Nebula System of M33

Ciardullo, Robin; Durrell, Patrick R.; Laychak, Mary Beth; Herrmann, Kimberly A.; Moody, Kenneth; Jacoby, George H.; Feldmeier, John J.

doi:10.1086/423414

Cited by 108 publications

(199 citation statements)

References 118 publications

(198 reference statements)

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“…The average AD is 11 ± 8% of V OIII max , which is similar to other measurements of local disk galaxies (e.g. Ciardullo et al 2004;Herrmann & Ciardullo 2009) and comparable to measurements in the solar neighborhood of the Milky Way (e.g. Ratnatunga & Upgren 1997;Olling & Dehnen 2003).…”

Section: Parameterized Rotation Curvessupporting

confidence: 88%

The DiskMass Survey

Martinsson

Verheijen

Westfall

et al. 2013

A&A

116

127

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We present ionized-gas ([Oiii]λ5007 Å) and stellar kinematics (velocities and velocity dispersions) for 30 nearly face-on spiral galaxies out to as many as three K-band disk scale lengths (h R ). These data have been derived from PPak integral-field-unit spectroscopy from 4980−5370 Å observed at a mean resolution of λ/Δλ = 7700 (σ inst = 17 km s −1 ). These data are a fundamental product of our survey and will be used in companion papers to, e.g., derive the detailed (baryonic+dark) mass budget of each galaxy in our sample. Our presentation provides a comprehensive description of the observing strategy and data reduction, including a robust measurement and removal of shift, scale, and rotation effects in the data due to instrumental flexure. Using an in-plane coordinate system determined by fitting circular-speed curves to our velocity fields, we derive azimuthally averaged rotation curves and line-of-sight velocity dispersion (σ LOS ) and luminosity profiles for both the stars and [Oiii]-emitting gas. Along with a clear presentation of the data, we demonstrate: (1) The [Oiii] and stellar rotation curves exhibit a clear signature of asymmetric drift with a rotation difference that is 11% of the maximum rotation speed of the galaxy disk, comparable to measurements in the solar neighborhood in the Milky Way.(2) The e-folding length of the stellar velocity dispersion (h σ ) is 2h R on average, as expected for a disk with a constant scale height and mass-to-light ratio, with a scatter that is notably smaller for massive, high-surface-brightness disks in the most luminous galaxies. (3) At radii larger than 1.5h R , σ LOS tends to decline slower than the best-fitting exponential function, which may be due to an increase in the disk mass-to-light ratio, disk flaring, or disk heating by the dark-matter halo. (4) A strong correlation exists between the central vertical stellar velocity dispersion of the disks (σ z,0 ) and their circular rotational speed at 2.2h R (V OIII 2.2h R ), with a zero point indicating that galaxy disks are submaximal. Moreover, weak but consistent correlations exist between σ z,0 /V OIII 2.2h R and global galaxy properties such that disks with a fainter central surface brightness in bluer and less luminous galaxies of later morphological types are kinematically colder with respect to their rotational velocities.

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Section: Parameterized Rotation Curvessupporting

confidence: 88%

The DiskMass Survey

Martinsson

Verheijen

Westfall

et al. 2013

A&A

116

127

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“…For instance in Fig. 6 of Ciardullo et al (2004) one could see evidence of two dips in their PNLF. In the present work we only confirm one dip at 22.9 mag, in accordance with their second dip, which is the sharper.…”

Section: The Sample Of Galaxiesmentioning

confidence: 99%

A two-mode planetary nebula luminosity function

Rodríguez-González

Hernández-Martínez

Esquivel

et al. 2015

A&A

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Context. We propose a new planetary nebula luminosity function (PNLF) that includes two populations in the distribution. Our PNLF is a direct extension of the canonical function proposed by Jacoby et al. (1987), in order to avoid problems related with the histogram construction, it is cast in terms of cumulative functions. Aims. We are interested in recovering the shape of the faint part of the PNLF in a consistent manner, for galaxies with and without a dip in their PNLFs. Methods. The parameters for the two-mode PNLF are obtained with a genetic algorithm, which obtains a best fit to the PNLF varying all of the parameters simultaneously in a broad parameter space. Results. We explore a sample of nine galaxies with various Hubble types and construct their PNLF. All of the irregular galaxies, except one, are found to be consistent with a two-mode population, while the situation is less clear for ellipticals and spirals.For the case of NGC 6822, we show that the two-mode PNLF is consistent with previous studies of the star formation history within that galaxy. Our results support two episodes of star formation, in which the second episode is significantly stronger.

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“…11, can be compared with those derived previously using different methods. The dynamical analysis of planetary nebulae in M 33 (Ciardullo et al 2004) yields mass-tolight ratios that increase radially, being 0.2 M /L V at R = 2 kpc and 0.8 M /L V at 5 kpc. However, this result is based on the assumption of radially constant vertical scaleheight and of a much longer radial scalelength of the stellar surface density than suggested by near-infrared photometry.…”

Section: The Surface Density Of the Baryonsmentioning

confidence: 99%

Dynamical signatures of a ΛCDM-halo and the distribution of the baryons in M 33

Corbelli

Thilker

Zibetti

et al. 2014

A&A

153

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Aims. We determine the mass distribution of stars, gas, and dark matter in M 33 to test cosmological models of galaxy formation and evolution. Methods. We map the neutral atomic gas content of M 33 using high resolution Very Large Array and Green Bank Telescope observations of the 21 cm HI line emission. A tilted ring model is fitted to the HI datacube to determine the varying spatial orientation of the extended gaseous disk and the rotation curve. We derive the stellar mass surface density map of M 33's optical disk via pixel-SED fitting methods based on population synthesis models that allow for positional changes in star formation history. Stellar and gas maps are used in the dynamical analysis of the rotation curve to constrain the dark halo properties. Results. The disk of M 33 warps from 8 kpc outward without substantial change of its inclination with respect to the line of sight; the line of nodes rotates clockwise toward the direction of M 31. Rotational velocities rise steeply with radius in the inner disk, reaching 100 km s −1 in 4 kpc, then the rotation curve becomes more perturbed and flatter with velocities as high as 120-130 km s −1 out to 2.7 R 25 . The stellar surface density map highlights a star-forming disk with a varying mass-to-light ratio. At larger radii, a dynamically relevant fraction of the baryons are in gaseous form. A dark matter halo with a Navarro-Frenk-White density profile, as predicted by hierarchical clustering and structure formation in a ΛCDM cosmology, provides the best fits to the rotation curve. Dark matter is relevant at all radii in shaping the rotation curve and the most likely dark halo has a concentration C 9.5 and a total mass of 4.3(±1.0) × 10 11 M . This imples a baryonic fraction of order 0.02 and the evolutionary history of this galaxy should therefore account for loss of a large fraction of its original baryonic content.

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The Planetary Nebula System of M33

Cited by 108 publications

References 118 publications

The DiskMass Survey

The DiskMass Survey

A two-mode planetary nebula luminosity function

Dynamical signatures of a ΛCDM-halo and the distribution of the baryons in M 33

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