RESONANT STRUCTURE IN THE DISKS OF SPIRAL GALAXIES, USING PHASE REVERSALS IN STREAMING MOTIONS FROM TWO-DIMENSIONAL Hα FABRY-PEROT SPECTROSCOPY

Font, J.; Beckman, J. E.; Épinat, B.; Fathi, Kambiz; Gutiérrez, L.; Hernandez, O.

doi:10.1088/2041-8205/741/1/l14

Cited by 38 publications

(47 citation statements)

References 27 publications

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“…It is widely accepted, from both observations and modeling, that the rotational parameter increases from early-to late-type galaxies (Aguerri et al 1998;Rautiainen et al 2008;Font et al 2011Font et al , 2014a. This could induce a misinterpretation of the histogram of this parameter (left panel of Figure 3) in which each peak could be erroneously associated with a particular morphological type of galaxy if only the mean value of this parameter were taken into account.…”

Section: Statistics Of the Bar Parametersmentioning

confidence: 99%

“…In this article we determine the bar corotation radius (and hence its pattern speed) with the Font-Beckman method (Font et al 2011(Font et al , 2014a, which uses phase-reversals of the streaming motions. In essence, from the line-of-sight velocity field in Hα we extract the rotation curve, which is used to construct a 2D model of the circular velocity, which is then subtracted from the original velocity field in order to produce the residual velocity map.…”

Section: The Corotation Radius Of the Bar And The Pattern Speedmentioning

confidence: 99%

“…They are (i) the well-known Tremaine-Winberg method (Tremaine & Weinberg 1984); its later modification to include multiple density wave patterns (Meidt et al 2008a(Meidt et al , 2008b combines photometric data with velocities derived from long-slit spectra placed parallel to the galaxy major axis (Kent 1987;Merrifield & Kruijken 1995;Gerssen et al 1999;Debattista et al 2002;Aguerri et al 2003;Corsini et al 2003;Debattista & Williams 2004;Rand & Wallin 2004;Zimmer et al 2004;Hernandez et al 2005;Fathi et al 2009;Corsini 2011, and references therein, Aguerri et al 2015). (ii) the gravitational potential distribution to reproduce the velocity map (Sanders & Tubbs 1980;England et al 1990;Garcia-Burillo et al 1993;Piñol-Ferrer et al 2014); (iii) the morphologies of the non-circular velocity map of the gas in the galaxy can be used (Canzian 1993;Rand 1995;Sempere et al 1995;Canzian & Allen 1997;Font et al 2011Font et al , 2014aFont et al , 2014b; (iv) finally, numerical simulations of barred galaxies are another method (Lindblad et al 1996;Laine & Heller 1999;Aguerri et al 2001;Weiner et al 2001;Pérez et al 2004;Rautiainen et al 2005Rautiainen et al , 2008Treuthardt et al 2008).…”

Section: Introductionmentioning

confidence: 99%

“…A quantitative step forward in terms of the number of galaxies measured was made by Font & Beckman (Font et al 2011, 2014a, 2014b, who took full advantage of the high spectral and spatial resolution made possible with scanning Fabry-Pérot spectroscopic technology to analyze the twodimensional velocity fields of over 100 galaxies observed in Hα. Instead of trying to determine the pattern speeds of the structures in these galaxies, the authors directed their attention directly to measuring the corotation radius (to be precise, the corotation radii, as they found radii associated with more than one structural component of the disk in virtually all cases).…”

Section: Introductionmentioning

confidence: 99%

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Kinematic Clues to Bar Evolution for Galaxies in the Local Universe: Why the Fastest Rotating Bars are Rotating Most Slowly

Font

Beckman

Martínez-Valpuesta

et al. 2017

ApJ

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We have used Spitzer images of a sample of 68 barred spiral galaxies in the local universe to make systematic measurements of bar length and bar strength. We combine these with precise determinations of the corotation radii associated with the bars, taken from our previous study, which used the phase change from radial inflow to radial outflow of gas at corotation, based on high-resolution two-dimensional velocity fields in Hα taken with a FabryPérot spectrometer. After presenting the histograms of the derived bar parameters, we study their dependence on the galaxy morphological type and on the total stellar mass of the host galaxy, and then produce a set of parametric plots. These include the bar pattern speed versus bar length, the pattern speed normalized with the characteristic pattern speed of the outer disk versus the bar strength, and the normalized pattern speed versus , the ratio of corotation radius to bar length. To provide guidelines for our interpretation, we used recently published simulations, including disk and dark matter halo components. Our most striking conclusion is that bars with values of  < 1.4, previously considered dynamically fast rotators, can be among the slowest rotators both in absolute terms and when their pattern speeds are normalized. The simulations confirm that this is because as the bars are braked, they can grow longer more quickly than the outward drift of the corotation radius. We conclude that dark matter halos have indeed slowed down the rotation of bars on Gyr timescales.

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Section: Statistics Of the Bar Parametersmentioning

confidence: 99%

Section: The Corotation Radius Of the Bar And The Pattern Speedmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Kinematic Clues to Bar Evolution for Galaxies in the Local Universe: Why the Fastest Rotating Bars are Rotating Most Slowly

Font

Beckman

Martínez-Valpuesta

et al. 2017

ApJ

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“…The GHαFaS instrument has been operative since 2007 , and has been used to study pattern speeds of bars and spiral arms (Fathi et al 2009), to analyse the kinematics of planetary nebulae (Santander-García et al 2010), and the gas flows (Font et al 2011b), star formation and the kinematics of interacting galaxies (Zaragoza-Cardiel et al 2013 and starburst galaxies (Blasco-Herrera et al 2013). It has also been used to study the resonance radii and interlocking resonance patterns in galaxy discs (Font et al 2011a(Font et al , 2014a.…”

mentioning

confidence: 99%

Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

Erroz-Ferrer¹,

Knapen²,

Leaman³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present a kinematical study of 29 spiral galaxies included in the Spitzer Survey of Stellar Structure in Galaxies, using Hα Fabry-Perot data obtained with the Galaxy Hα Fabry-Perot System instrument at the William Herschel Telescope in La Palma, complemented with images in the R band and in Hα. The primary goal is to study the evolution and properties of the main structural components of galaxies through the kinematical analysis of the FP data, complemented with studies of morphology, star formation and mass distribution. In this paper we describe how the FP data have been obtained, processed and analysed. We present the resulting moment maps, rotation curves, velocity model maps and residual maps. Images are available in FITS format through the NASA/IPAC Extragalactic Database and the Centre de Données Stellaires. With these data products we study the non-circular motions, in particular those found along the bars and spiral arms. The data indicate that the amplitude of the non-circular motions created by the bar does not correlate with the bar strength indicators. The amplitude of those non-circular motions in the spiral arms does not correlate with either arm class or star formation rate along the spiral arms. This implies that the presence and the magnitude of the streaming motions in the arms is a local phenomenon.

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A model for the Lin‐Shu type density‐wave structure of our Galaxy: Line‐of‐sight and transverse‐longitudinal velocities of 242 optically visible open clusters

Griv

Jiang

2015

Astron Nachr

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In this paper, the fourth in a series, we examine again one of the implications of the Lin-Shu density-wave theory, specifically, the noncircular systematic motion of the Galactic objects. Our previous investigation is extended by analyzing simultaneously both the line-of-sight and transversal velocities of a sample of open clusters for which velocities, distances and ages are available. The ordinary equations of the Oort-Lindblad theory of galactic differential rotation are used. The minor effects caused by the two-dimensional tightly-wound density waves are also taken into account. The published data of 242 currently known optically visible clusters having distances r < 3 kpc from the Sun and −200 < z < 200 pc from the Galactic plane, and ages 2×10 8 < t < 2×10 9 yr are collected from Dias et al. (2014), excluding extremely far, high-velocity, young and old objects in our fitting. The most noteworthy result is the fact that the parameters of Lin-Shu type density waves estimated from two independent line-of-sight and transversal along the Galactic longitude velocities are nearly equal. We argue that the resemblance of these Galactic wave structures is so remarkable that no doubt is felt as to the theory's truth with respect to these data. The results obtained allow us to conclude that several low-m trailing density-wave patterns with different number of spiral arms m (say, m = 1, 2, 3, and 4), pitch angles (about 5• , 8• , 11• , and 14 • , respectively) and amplitudes of the perturbed gravitational potential may coexist in the Galaxy. The latter suggests the asymmetric multiarm, not well-organized ("flocculent") spiral structure of the system.

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RESONANT STRUCTURE IN THE DISKS OF SPIRAL GALAXIES, USING PHASE REVERSALS IN STREAMING MOTIONS FROM TWO-DIMENSIONAL Hα FABRY-PEROT SPECTROSCOPY

Cited by 38 publications

References 27 publications

Kinematic Clues to Bar Evolution for Galaxies in the Local Universe: Why the Fastest Rotating Bars are Rotating Most Slowly

Kinematic Clues to Bar Evolution for Galaxies in the Local Universe: Why the Fastest Rotating Bars are Rotating Most Slowly

Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

A model for the Lin‐Shu type density‐wave structure of our Galaxy: Line‐of‐sight and transverse‐longitudinal velocities of 242 optically visible open clusters

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