As parentológicas Arawá e Arawak: um estudo sobre parentesco e aliança

Florido, Marcelo Pedro

doi:10.11606/d.8.2008.tde-22012009-173530

Cited by 8 publications

(12 citation statements)

References 7 publications

(9 reference statements)

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“…Taking a g /a * ∼ .2, and H * of the order of one kiloparsec, we find an order of magnitude of one kiloparsec for the wavelength of the corrugation. This is consistent with the observed wavelength for the corrugation, in the Milky Way (Quiroga andSchlosser 1977, Spicker andFeitzinger 1986) or in other galaxies (Florido et al 1991a). Despite the observations by Spicker and Feitzinger of a one kiloparsec corrugation in our galaxy, it seems that the typical wavelength of corrugation is rather about 2 kiloparsecs, or even larger (Florido et al 1991b).…”

Section: Expected Characteristics Of the Corrugationsupporting

confidence: 90%

“…This is consistent with the observed wavelength for the corrugation, in the Milky Way (Quiroga andSchlosser 1977, Spicker andFeitzinger 1986) or in other galaxies (Florido et al 1991a). Despite the observations by Spicker and Feitzinger of a one kiloparsec corrugation in our galaxy, it seems that the typical wavelength of corrugation is rather about 2 kiloparsecs, or even larger (Florido et al 1991b). The discrepancy of 2 between observations and our estimate could be due either to the magnetic field which affects the gas motions and thus should imply the use of magnetosonic speeds instead of the acoustic speed, or to a lack of resolution of some observations.…”

Section: Expected Characteristics Of the Corrugationsupporting

confidence: 90%

“…We would have only one wave emitted outward and two inwards, but the order of magnitude of their amplitudes would not change. Note that observations of corrugation in external galaxies (Florido et al 1991a) seem to reveal two distinct wavelength for corrugation waves.…”

Section: What About the Halo ?mentioning

confidence: 89%

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Non-Linear Excitation of Warps by Spiral Waves in Galaxies

Masset¹,

Tagger²

1996

International Astronomical Union Colloquium

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Abstract.We present a mechanism to explain the permanent excitation of warps in spiral or barred galaxies. We show that non-linear mode coupling with the spiral wave can be very efficient to drive two warp waves. We derive an expression of the coupling coefficient in the WKB approximation. We show that the coupling is too weak in the stellar disk, except at the Outer Lindblad Resonance where the spiral slows down and is efficiently coupled to warp waves. There, the spiral can almost completely transfer its energy and angular momentum to a "transmitted" warp, which we can observe in HI, and a "reflected" one, which we can observe as a corrugation. Our mechanism reproduces the observed amplitudes of the warp and of the corrugation.We first present side results concerning the propagation of warps in moderately thick disks. Linear results: Propagation of Warps in Moderately Thick DisksIn an infinitely thin disk, the dispersion relation of bending waves is: a) 2 = fj, 2 + 27rG£fc, where UJ is the warp's frequency in the frame of matter (if ui is its frequency in the galactocentric frame,

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Section: Expected Characteristics Of the Corrugationsupporting

confidence: 90%

Section: Expected Characteristics Of the Corrugationsupporting

confidence: 90%

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Non-Linear Excitation of Warps by Spiral Waves in Galaxies

Masset¹,

Tagger²

1996

International Astronomical Union Colloquium

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“…It is of the Sb type, with several outstanding features which were studied by different authors. The galaxy has a barely visible optical warp (Florido et al 1991). Martínez-Delgado et al (2009) found a giant, arcing stellar structure of low surface brightness around the galaxy.…”

Section: Ngc 4013mentioning

confidence: 99%

HERschelObservations of Edge-on Spirals (HEROES)

Mosenkov

Allaert

Baes

et al. 2018

A&A

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We present results of the detailed dust energy balance study for the seven large edge-on galaxies in the HEROES sample using 3D radiative transfer (RT) modelling. Based on available optical and near-infrared observations of the HEROES galaxies, we derive the 3D distribution of stars and dust in these galaxies. For the sake of uniformity, we apply the same technique to retrieve galaxy properties for the entire sample: we use a stellar model consisting of a Sérsic bulge and three double-exponential discs (a superthin disc for a young stellar population and thin and thick discs for old populations). For the dust component, we adopt a double-exponential disc with the new THEMIS dust-grain model. We fit oligochromatic radiative transfer (RT) models to the optical and near-infrared images with the fitting algorithm fitskirt and do panchromatic simulations with the skirt code at wavelengths ranging from ultraviolet to submillimeter. We confirm the previously stated dust energy balance problem in galaxies: for the HEROES galaxies, the dust emission derived from our RT calculations underestimates the real observations by a factor 1.5-4 for all galaxies except NGC 973 and NGC 5907 (apparently, the latter galaxy has a more complex geometry than we used). The comparison between our RT simulations and the observations at mid-infrared-submillimeter wavelengths shows that most of our galaxies exhibit complex dust morphologies (possible spiral arms, star-forming regions, more extended dust structure in the radial and vertical directions). We suggest that, in agreement with the results from Saftly et al. (2015), the large-and small-scale structure is the most probable explanation for the dust energy balance problem.

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“…See Figure 14 for typical examples of S or Z-shaped morphology. In an early compilation Florido et al (1990) found approximately 11% of radio sources with two jets showed S or Z-shaped morphology while approximately 9% showed both jets curving in same direction. The sample was 365 sources from published observations.…”

Section: S or Z-shapementioning

confidence: 99%

Morphological Annotations for Groups in the First Database

Proctor

2011

ApJS

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The morphology of selected groups of sources in the FIRST (Faint Images of the Radio Sky at Twenty Centimeters) survey and catalog is examined. Sources in the FIRST catalog (April 2003 release, 811117 entries) were sorted into singles, doubles, triples and groups of higher-count membership based on a proximity criteria. The 7106 groups with four or more components were examined individually for bent types including, but not limited to, wide-angle tail (WAT) and narrowangle tail (NAT) types. In the process of this examination, ring, double-double (DD), X-shaped, hybrid morphology (HYMOR), giant radio sources (GRS), and the herein described W-shaped and tri-axial morphology systems were also identified. For the convenience of the reader separate tables for distinctive types were generated. A few curiosities were found. For the 16,950 three-component groups and 74,788 two-component groups, catalogs with probability estimates for bent classification, as determined by pattern recognition techniques, are presented.

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As parentológicas Arawá e Arawak: um estudo sobre parentesco e aliança

Cited by 8 publications

References 7 publications

Non-Linear Excitation of Warps by Spiral Waves in Galaxies

Non-Linear Excitation of Warps by Spiral Waves in Galaxies

HERschelObservations of Edge-on Spirals (HEROES)

Morphological Annotations for Groups in the First Database

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