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Journal articles on the topic 'Cartwheel galaxy'

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Author: Grafiati

Published: 9 March 2023

Last updated: 10 March 2023

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1

Bosma, A. "Models of the Cartwheel Galaxy." International Astronomical Union Colloquium 174 (2000): 255–60. http://dx.doi.org/10.1017/s0252921100055081.

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2

Crivellari, E., A. Wolter, and G. Trinchieri. "The Cartwheel galaxy with XMM-Newton." Astronomy & Astrophysics 501, no. 2 (May 13, 2009): 445–53. http://dx.doi.org/10.1051/0004-6361/200810707.

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3

Struck-Marcell, Curtis, and James L. Higdon. "Hydrodynamic models of the Cartwheel ring galaxy." Astrophysical Journal 411 (July 1993): 108. http://dx.doi.org/10.1086/172811.

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4

Griv, Evgeny. "Origin of the Cartwheel Galaxy: Disk Instability?" Astrophysics and Space Science 299, no. 4 (October 2005): 371–85. http://dx.doi.org/10.1007/s10509-005-3423-5.

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5

Banks, Michael. "James Webb Space Telescope image peers into the chaos of the Cartwheel galaxy." Physics World 35, no. 9 (November 1, 2022): 9ii. http://dx.doi.org/10.1088/2058-7058/35/09/11.

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6

Trinchieri, Ginevra, Anna Wolter, and Angela Iovino. "A Ring of X-rays from the Cartwheel Galaxy." International Astronomical Union Colloquium 166 (1997): 551–54. http://dx.doi.org/10.1017/s0252921100071591.

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AbstractROSAT HRI observations of the Cartwheel galaxy indicate that there is X-ray emission from the outer ring in connection with the strongest HII regions in the southern portion of the ring. No significant emission is detected from the nucleus or from the inner ring. This implies a strong connection between star formation activity and X-ray emission in this ring galaxy.

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7

Barway, Sudhanshu, Y. D. Mayya, and Aitor Robleto-Orús. "Discovery of a near-infrared bar and a pseudo-bulge in the collisional ring galaxy Cartwheel." Monthly Notices of the Royal Astronomical Society 497, no. 1 (July 3, 2020): 44–51. http://dx.doi.org/10.1093/mnras/staa1887.

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ABSTRACT We report the discovery of a bar, a pseudo-bulge, and unresolved point source in the archetype collisional ring galaxy Cartwheel using careful morphological analysis of a near-infrared (NIR) Ks-band image of excellent quality (seeing = 0.42″) at the ESO archive. The bar is oval-shaped with a semi-major axis length of 3.23″ (∼2.09 kpc), with almost a flat light distribution along it. The bulge is almost round (ellipticity = 0.21) with an effective radius of 1.62″ (∼1.05 kpc) and a Sersic index of 0.99, parameters typical of pseudo-bulges in late-type galaxies. The newly discovered bar is not recognizable as such in the optical images even with more than a factor of 2 higher spatial resolution of the Hubble Space Telescope, due to a combination of its red colour and the presence of dusty features. The observed bar and pseudo-bulge most likely belonged to the pre-collisional progenitor of the Cartwheel. The discovery of a bar in an archetype collisional ring galaxy Cartwheel is the first observational evidence to confirm the prediction that bars can survive a drop-through collision along with the morphological structures like a central bulge (pseudo).

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8

Wolter, Anna, Guido Consolandi, Marcella Longhetti, Marco Landoni, and Andrea Bianco. "The Cartwheel galaxy as a stepping stone for binaries formation." Proceedings of the International Astronomical Union 14, S346 (August 2018): 297–306. http://dx.doi.org/10.1017/s1743921319001157.

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AbstractUltraluminous X-ray sources (ULXs) are end points of stellar evolution. They are mostly interpreted as binary systems with a massive donor. They are also the most probable progenitors for BH-BH, and even more, for BH-NS coalescence. Parameters of ULXs are not know and need to be better determined, in particular the link with the metallicity of the environment which has been invoked frequently but not proven strongly. We have tackled this problem by using a MUSE DEEP mosaic of the Cartwheel galaxy and applying a Monte Carlo code that jointly fits spectroscopy and photometry. We measure the metallicity of the emitting gas in the ring and at the positions of X-ray sources by constructing spatially resolved emission line ratio maps and BPT diagnostic maps. The Carthweel is the archetypal ring galaxy and the location and formation time of new stellar populations is easier to reconstruct than in more normal galaxies. It has the largest population of ULXs ever observed in a single galaxy (16 sources have been classified as ULXs in Chandra and XMM-Newton data). The Cartwheel galaxy is therefore the ideal laboratory to study the relation between Star Formation (SF Rates and SF History) and number of ULXs and also their final fate. We find that the age of the stellar population in the outer ring is consistent with being produced in the impact (≤300Myr) and that the metallicity is mostly sub-solar, even if solutions can be found with a solar metallicity that account for most observed properties. The findings for the Cartwheel will be a testbed for further modelisation of binary formation and evolution paths.

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9

Soria, R., M. S. Cropper, and M. W. Pakull. "A ULX in NGC 4559: A “Mini-Cartwheel” Scenario?" International Astronomical Union Colloquium 194 (2004): 57–59. http://dx.doi.org/10.1017/s0252921100151905.

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AbstractWe have studied the peculiar environment around a ULX in NGC 4559 (with Lx ≈ 2 x 1040 erg s–1 and MBH ≳ 50M⊙). The X-ray source is located near the rim of a young (age < 30 Myr), large (diameter ≈ 700 pc) ring-like star forming complex possibly triggered by the impact of a dwarf satellite galaxy through the gas-rich outer disk of NGC 4559. We speculate that galaxy interactions (including the infall of high-velocity clouds and satellites on a galactic disk) and low-metallicity environments offer favourable conditions for the formation of compact remnants more massive than “standard” X-ray binaries, and accreting from a massive Roche-lobe filling companion.

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10

Renaud, F., E. Athanassoula, P. Amram, A. Bosma, F. Bournaud, P. A. Duc, B. Epinat, et al. "Morphology and enhanced star formation in a Cartwheel-like ring galaxy." Monthly Notices of the Royal Astronomical Society 473, no. 1 (September 12, 2017): 585–602. http://dx.doi.org/10.1093/mnras/stx2360.

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11

Higdon, James L. "Wheels of Fire. II. Neutral Hydrogen in the Cartwheel Ring Galaxy." Astrophysical Journal 467 (August 1996): 241. http://dx.doi.org/10.1086/177599.

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12

Vorobyov, E. I., V. I. Korchagin, and Y. D. Mayya. "Optical and near-ir color gradients in the Cartwheel ring galaxy." Astronomical & Astrophysical Transactions 20, no. 2 (August 2001): 247–51. http://dx.doi.org/10.1080/10556790108229705.

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13

Horellou, C. "Collisional Ring Galaxies in Small Groups." International Astronomical Union Colloquium 174 (2000): 277–80. http://dx.doi.org/10.1017/s0252921100055111.

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AbstractThe probability of plunging orbits is enhanced in groups of galaxies and indeed, observations show that ring galaxies, which are believed to form when a galaxy passes through the center of a larger rotating disk, are often found in small groups. Numerical simulations combined with a knowledge of the large-scale H I distribution provide strong constraints on the dynamical history of these systems and on the identity of the intruder. Here we present a numerical model of the Cartwheel galaxy which supports the suggestion that the most distant companion is the intruder. We also present high-resolution H I observations of the more irregular system Arp 119 that reveal a possible connection to the most distant companion.

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14

Gao, Yu, Q. Daniel Wang, P. N. Appleton, and Ray A. Lucas. "Nonnuclear Hyper/Ultraluminous X-Ray Sources in the Starbursting Cartwheel Ring Galaxy." Astrophysical Journal 596, no. 2 (September 29, 2003): L171—L174. http://dx.doi.org/10.1086/379598.

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15

Mapelli, M., M. Colpi, and L. Zampieri. "Low metallicity and ultra-luminous X-ray sources in the Cartwheel galaxy." Monthly Notices of the Royal Astronomical Society: Letters 395, no. 1 (May 1, 2009): L71—L75. http://dx.doi.org/10.1111/j.1745-3933.2009.00645.x.

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16

Higdon, James L. "Wheels of Fire. I. Massive Star Formation in the Cartwheel Ring Galaxy." Astrophysical Journal 455 (December 1995): 524. http://dx.doi.org/10.1086/176602.

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17

Vorobyov, E. I. "Large-scale ring waves of star formation in the cartwheel ring galaxy." Astronomical & Astrophysical Transactions 22, no. 1 (February 2003): 95–102. http://dx.doi.org/10.1080/1055679021000017376.

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18

Hosseinzadeh, Griffin, David J. Sand, Jacob E. Jencson, Jennifer E. Andrews, Irene Shivaei, K. Azalee Bostroem, Stefano Valenti, et al. "JWST Imaging of the Cartwheel Galaxy Reveals Dust Associated with SN 2021afdx." Astrophysical Journal Letters 942, no. 1 (January 1, 2023): L18. http://dx.doi.org/10.3847/2041-8213/aca64e.

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Abstract We present near- and mid-infrared (0.9–18 μm) photometry of supernova (SN) 2021afdx, which was imaged serendipitously with the James Webb Space Telescope (JWST) as part of its Early Release Observations of the Cartwheel Galaxy. Our ground-based optical observations show it is likely to be a Type IIb SN, the explosion of a yellow supergiant, and its infrared spectral energy distribution (SED) ≈200 days after explosion shows two distinct components, which we attribute to hot ejecta and warm dust. By fitting models of dust emission to the SED, we derive a dust mass of ( 3.8 − 0.3 + 0.5 ) × 10 − 3 M ⊙ , which is the highest yet observed in a Type IIb SN but consistent with other Type II SNe observed by the Spitzer Space Telescope. We also find that the radius of the dust is significantly larger than the radius of the ejecta, as derived from spectroscopic velocities during the photospheric phase, which implies that we are seeing an infrared echo off of preexisting dust in the progenitor environment, rather than dust newly formed by the SN. Our results show the power of JWST to address questions of dust formation in SNe, and therefore the presence of dust in the early universe, with much larger samples than have been previously possible.

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19

Wolter, Anna, Ginevra Trinchieri, and Monica Colpi. "Variability of ultraluminous X-ray sources in the Cartwheel Ring." Proceedings of the International Astronomical Union 2, S238 (August 2006): 255–58. http://dx.doi.org/10.1017/s174392130700508x.

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AbstractThe Cartwheel is one of the most outstanding examples of a dynamically perturbed galaxy where star formation is occurring inside the ring–like structure. In previous studies with Chandra, we detected 16 Ultra Luminous X-ray sources lying along the southern portion of the ring. Their Luminosity Function is consistent with them being in the high luminosity tail of the High Mass X-ray Binaries distribution, but with one exception: source N.10. This source, detected with Chandra at LX = 1 × 1041 erg s−1, is among the brightest non–nuclear sources ever seen in external galaxies. Recently, we have observed the Cartwheel with XMM-Newton in two epochs, six months apart. After having been at its brightest for at least 4 years, the source has dimmed by at least a factor of two between the two observations. This fact implies that the source is compact in nature. Given its extreme isotropic luminosity, there is the possibility that the source hosts an accreting intermediate–mass black hole. Other sources in the ring vary in flux between the different datasets. We discuss our findings in the context of ULX models.

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20

Mapelli, M., B. Moore, L. Giordano, L. Mayer, M. Colpi, E. Ripamonti, and S. Callegari. "Intermediate-mass black holes and ultraluminous X-ray sources in the Cartwheel ring galaxy." Monthly Notices of the Royal Astronomical Society 383, no. 1 (December 5, 2007): 230–46. http://dx.doi.org/10.1111/j.1365-2966.2007.12534.x.

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21

Castillo Rosales, Yvelice Soraya. "First James Webb Space Telescope´s images." Innovare: Revista de ciencia y tecnología 11, no. 2 (August 30, 2022): 111. http://dx.doi.org/10.5377/innovare.v11i2.14787.

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From left to right and from top to bottom: 1. The Stephan's Quintet (interacting galaxies' group), 40 million and 290 million light-years away; 2. The Cartwheel Galaxy, a merger of galaxies of 144,300 light-years across, 500 million light-years away; 3. The spectrum of the exoplanet WASP-96b (1,150 light-years away), showing evaporated water; 4. James Webb telescope in its clean room; 5. The South Ring Nebula, 2,500 light-years away (12 light-years across); 6. Galactic cluster in the early universe SMACS 07323, 4,600,000,000 light-years away; 7. The star formation region NGC 3324 (Gabriela Mistral) in the Carina Nebula (NGC3372), 7,600 light-years away.

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22

Struck, Curtis, Philip N. Appleton, Kirk D. Borne, and Ray A. Lucas. "Hubble Space Telescope Imaging of Dust Lanes and Cometary Structures in the Inner Disk of the Cartwheel Ring Galaxy." Astronomical Journal 112 (November 1996): 1868. http://dx.doi.org/10.1086/118148.

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23

Vorobyov, E. I., and D. Bizyaev. "Radial $B-V/V-K$ color gradients, extinction-freeQBVKcombined color indices, and the history of star formation of the Cartwheel ring galaxy." Astronomy & Astrophysics 377, no. 3 (October 2001): 835–44. http://dx.doi.org/10.1051/0004-6361:20011163.

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24

Marcum, P. M., P. N. Appleton, and J. L. Higdon. "Large infrared and optical color gradients in the Cartwheel ring galaxy - Evidence for the first epoch of star formation in the wake of an expanding ring." Astrophysical Journal 399 (November 1992): 57. http://dx.doi.org/10.1086/171902.

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25

Zaragoza-Cardiel, Javier, V. Mauricio A. Gómez-González, Divakara Mayya, and Gerardo Ramos-Larios. "Nebular abundance gradient in the Cartwheel galaxy using MUSE data." Monthly Notices of the Royal Astronomical Society, May 24, 2022. http://dx.doi.org/10.1093/mnras/stac1423.

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Abstract We here present the results from a detailed analysis of nebular abundances of commonly observed ions in the collisional ring galaxy Cartwheel using the Very Large Telescope (VLT) Multi-Unit Spectroscopic Explorer (MUSE) dataset. The analysis includes 221 H ii regions in the star-forming ring, in addition to 40 relatively fainter Hα-emitting regions in the spokes, disk and the inner ring. The ionic abundances of He, N, O and Fe are obtained using the direct method (DM) for 9, 20, 20, and 17 ring H ii regions, respectively, where the S++ temperature-sensitive line is detected. For the rest of the regions, including all the nebulae between the inner and the outer ring, we obtained O abundances using the strong-line method (SLM). The ring regions have a median $12+\log \rm {\frac{O}{H}}$ = 8.19 ± 0.15, $\log \rm {\frac{N}{O}} = -$1.57 ± 0.09 and $\log \rm {\frac{Fe}{O}} = -$2.24 ± 0.09 using the DM. Within the range of O abundances seen in the Cartwheel, the N/O and Fe/O values decrease proportionately with increasing O, suggesting local enrichment of O without corresponding enrichment of primary N and Fe. The O abundances of the disk H ii regions obtained using the SLM show a well-defined radial gradient. The mean O abundance of the ring H ii regions is lower by ∼0.1 dex as compared to the extrapolation of the radial gradient. The observed trends suggest the preservation of the pre-collisional abundance gradient, displacement of most of the processed elements to the ring, as predicted by the recent simulation by Renaud et al. (2018), and post-collisional infall of metal-poor gas in the ring.

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26

Pizzolato, Fabio, Anna Wolter, and Ginevra Trinchieri. "Chandra observations of the ULX N10 in the Cartwheel galaxy." Monthly Notices of the Royal Astronomical Society, April 2010, no. http://dx.doi.org/10.1111/j.1365-2966.2010.16735.x.

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27

Mayya, Y. D., A. Plat, V. M. A. Gómez-González, J. Zaragoza-Cardiel, S. Charlot, and G. Bruzual. "Detection of He++ ion in the star-forming ring of the Cartwheel using MUSE data and ionizing mechanisms." Monthly Notices of the Royal Astronomical Society, January 9, 2023. http://dx.doi.org/10.1093/mnras/stad017.

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Abstract We here report the detection of the nebular He ii λ4686 line in 32 H ii regions in the metal-poor collisional ring galaxy Cartwheel using the Multi-Unit Spectroscopic Explorer (MUSE) dataset. The measured I(He ii λ4686)/I(Hβ) ratio varies from 0.004 to 0.07, with a mean value of 0.010±0.003. Ten of these 32 H ii regions are coincident with the location of an Ultra Luminous X-ray (ULX) source. We used the flux ratios of important diagnostic lines and results of photoionization by Simple Stellar Populations (SSPs) to investigate the likely physical mechanisms responsible for the ionization of He+. We find that the majority of the regions (27) are consistent with photoionization by star clusters in their Wolf-Rayet (WR) phase with initial ionization parameter −3.5 <log 〈U〉<−2.0. Blue Bump (BB), the characteristic feature of the WR stars, however, is not detected in any of the spectra. We demonstrate that this non-detection is due to the relatively low equivalent width (EW) of the BB in metal-poor SSPs, in spite of containing sufficient number of WR stars to reproduce the observed I(He ii λ4686)/I(Hβ) ratio of ≤1.5 per cent at the Cartwheel metallicity of Z=0.004. The H ii regions in the WR phase that are coincident with a ULX source do not show line ratios characteristic of ionization by X-ray sources. However, the ULX sources may have a role to play in the ionization of He+ in two (#99, 144) of the five regions that are not in the WR phase. Ionization by radiative shocks along with the presence of channels for the selective leakage of ionizing photons are the likely scenarios in #17 and #148, the two regions with the highest observed I(He ii λ4686)/I(Hβ) ratio.

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