Central Rotation Curves of Spiral Galaxies

Sofue, Yoshiaki; Tutui, Y.; Honma, Mareki; Tomita, Akihiko; Takamiya, Tsutomu; Koda, Jin; Takeda, Yoichi

doi:10.1086/307731

Cited by 236 publications

(271 citation statements)

References 24 publications

(47 reference statements)

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“…(1) Helfer et al (2003); (2) Sofue et al (1999); (3) Lu et al (1993); (4) Zimmer et al (2004); (5) Kamphuis & Briggs (1992); (6) Moustakas et al (2010); (7) Cedrés et al (2004). Foyle et al (2010), using a multiband analysis from H I to the far-UV for the grand design galaxies NGC 5194, NGC 682, and NGC 6946, found that there is no shock trigger, and that the spiral arms just reorganize the material from the disc, which will generate stars as a function of gas density, following a KennicuttSchmidt law, for example (Kennicutt 1998a).…”

Section: Introductionmentioning

confidence: 99%

Density waves and star formation in grand-design spirals

Cedrés

Cepa

Bongiovanni

et al. 2013

A&A

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Context. H II regions in the arms of spiral galaxies are indicators of recent star-forming processes. They may have been caused by the passage of the density wave or simply been created by other means near the arms. The study of these regions may give us clues to clarify the controversy about the existence of a triggering scenario, as proposed in the density-wave theory. Aims. If the passage of the density wave contributes significantly to the formation of H II regions in the arms of grand-design spirals, we can find a relationship in their position relative to the arms. Methods. Using Hα direct imaging, we characterize the H II regions from a sample of three grand-design galaxies: NGC 5457, NGC 628, and NGC 6946. Broad-band images in R and I were used to determine the position of the arms. The H II regions found to be associated with arms were selected for the study. The age and star formation rate of these H II regions was obtained using measurements on the Hα line. The distance between the current position of the selected H II regions and the position they would have if they had been created in the centre of the arm was calculated. A parameter, T , which measures whether a region was created in the arm or in the disc, was defined. Results. With the help of the T parameter we determine that the majority of regions were formed some time after the passage of the density wave, and the regions are located behind the zone they should have occupied (in the direction of the rotation of the galaxy) had they been formed in the centre of the arm. Moreover, the relative efficiency of the star formation rate between arm and interarm was calculated for all the galaxies. Conclusions. The large number of regions created after the passage of the arm may be explained by the effect of the density wave, which helps to create the star-forming regions after its passage. There is clear evidence of triggering for NGC 5457 and a co-rotation radius is proposed. A more modest triggering seems to exist for NGC 628, and insignificant evidence of triggering is found for NGC 6946.

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Section: Introductionmentioning

confidence: 99%

Density waves and star formation in grand-design spirals

Cedrés

Cepa

Bongiovanni

et al. 2013

A&A

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Section: Galactic Rotation Curvesmentioning

confidence: 98%

“…Note that the velocity of stars does not decrease at high radius, but rather asymptotes to a constant, indicating an interior mass function M (r) ∝ r. As the luminous interior mass grows much more slowly than this, these curves imply contributions from a significant dark matter component [21]. [21]. A collection of galactic rotation curves from [21] can be seen in Figure 1-6, and Figure 1 -7 [22] shows the contributions of the luminous disk and the dark halo for NGC 3198 specifically.…”

Section: Galactic Rotation Curvesmentioning

confidence: 98%

“…[21]. A collection of galactic rotation curves from [21] can be seen in Figure 1-6, and Figure 1 -7 [22] shows the contributions of the luminous disk and the dark halo for NGC 3198 specifically. Rather than falling off at high radii, the velocity curves roughly asymptote to a constant for all stars outside of the central dense region, out to the furthest observable stars.…”

Section: Galactic Rotation Curvesmentioning

confidence: 99%

“…The ATLAS limits for operators involving quarks are for the four light flavours assuming equal coupling strengths for all quark flavours to the WIMPs. For comparison, 90% CL limits from the XENON100 [70], CDMSII [71], CoGeNT [72], CDF [19], and CMS [21] experiments are shown. scattering cross sections is done using equations (3) to (6) of ref.…”

Section: Production At Collidersmentioning

confidence: 99%

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Detector Simulation and WIMP Search Analysis for the Cryogenic Dark Matter Search Experiment

McCarthy¹

2013

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Astrophysical and cosmological measurements on the scales of galaxies, galaxy clusters, and the universe indicate that ∼85% of the matter in the universe is composed of dark matter, made up of non-baryonic particles that interact with cross-sections on the weak scale or lower. Hypothetical Weakly Interacting Massive Particles, or WIMPs, represent a potential solution to the dark matter problem, and naturally arise in certain Standard Model extensions.The Cryogenic Dark Matter Search (CDMS) collaboration aims to detect the scattering of WIMP particles from nuclei in terrestrial detectors. Germanium and silicon particle detectors are deployed in the Soudan Underground Laboratory in Minnesota. These detectors are instrumented with phonon and ionization sensors, which allows for discrimination against electromagnetic backgrounds, which strike the detector at rates orders of magnitude higher than the expected WIMP signal.This dissertation presents the development of numerical models of the physics of the CDMS detectors, implemented in a computational package collectively known as the CDMS Detector Monte Carlo (DMC). After substantial validation of the models against data, the DMC is used to investigate potential backgrounds to the next iteration of the CDMS experiment, known as SuperCDMS. Finally, an investigation of using the DMC in a reverse Monte Carlo analysis of WIMP search data is presented.140.23 kg-days of WIMP search data from the silicon detectors in the CDMSII experiment is also analyzed. The resulting upper limits on the WIMP-nucleon crosssection are higher than those published by other experiments at all WIMP masses, and the lowest limit on the WIMP-nucleon cross-section is 1.07*10 −42 cm 2 at a mass 3 of 60 GeV/c 2 . These results do provide new and interesting constraints at WIMP masses ≤40 GeV/c 2 and cross sections from 10 −42 -10 −39 cm 2 , a region in which some WIMP search experiments have claimed evidence for a WIMP signal, which other experiments claim to have ruled out.

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2014

Beyond the Standard Model of Elementary Particle Physics

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Central Rotation Curves of Spiral Galaxies

Cited by 236 publications

References 24 publications

Density waves and star formation in grand-design spirals

Density waves and star formation in grand-design spirals

Detector Simulation and WIMP Search Analysis for the Cryogenic Dark Matter Search Experiment

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