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| | GIC - Why things have been done in GIC |
 | | As is instantly seen Ngc 5236 is wrapped by dimly luminant ghost arms which extend the object well beyond its normally viewed optically brighter parts, and so form part of its superstructure. | | | The vortexing stretched out canister shape of such galaxies would not easily be inferred even sometime future until doppler red/blue shift velocity analysis was developed to an extreme high state of the art where interpretation would yield a cannister dramatically stretched out in space along a Z axis. | | | Even though grainy as hell, this next image serves well to illustrate just how thick Ngc 5236 actually is, so, add more mass to the mass already learned from analysing it's open cannister vortex shape in deep space. |
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http://www.cosmicastronomy.com/purpose.htm
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| | Deepsky observing report M16, M17, M18, M24, M22, M8, M11, IC 4756, NGC 6633, NGC 253, NGC 247, NGC 188, NGC 891 |
| | NGC 253 can be found about 7 to 8° to the south of this 2nd magnitude star. | | | With averted vision I could detect one or two foreground stars, superimposed on the outer edges of NGC 253. | | | I centred the finder-scope in a sort of trapezoid, formed by four stars (magnitude 6 to 7). |
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http://www.backyard-astro.com/deepsky/2003_09_26/ITT.html
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| | Galaxy Data |
| | NED data files for NGC 253 are updated regularly and carry bibliographic references. | | | NED data files for NGC 4322 and NGC 4323 are updated regularly and carry bibliographic references. | | | NED data files for NGC 5128 are updated regularly and carry bibliographic references. |
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http://pandora.nla.gov.au/pan/24870/20020715/www.aao.gov.au/images/general/galaxy_data.html
(5943 words)
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| | APOD Search Results for "NGC galaxies" |
| | NGC 6782 demonstrates colorfully that they do not. | | | At distance of a mere 8 million light-years, NGC 253's prodigious starforming activity has been well studied using high-resolution optical images like the one seen here at lower left. | | | The resulting turbulent environment is fed by supernova explosions as the cosmic detonations spew out material and trigger further star formation. |
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http://antwrp.gsfc.nasa.gov/cgi-bin/apod/apod_search?NGC+galaxies
(10664 words)
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| | DOC: Uranometria chart 306 |
| | THE SOUTHERN PORTION of the sweeping tail of Cetus the Sea Monster is shown on this chart, marked by the yellowish 2nd magnitude luminary Diphda (Beta Ceti). | | | The ESO/Uppsala Survey of the ESO(B) Atlas remarks: "In foreground of cluster." The magnitude is given as 9.4. | | | The error cannot lie in this observation, the 109th degree of Polar distance being beyond the possible reach of the instrument in [this] sweep." |
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http://www.fortunecity.com/roswell/borley/49/u306.htm
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| | NGC 253 Radio Images |
| | Another optical image of NGC 253, taken with the Anglo-Australian Telescope, is available from the Anglo-Australian Observatory Web site. | | | For comparison, here is an optical image of NGC 253. | | | This image is available as a downloadable GIF file for people with non-graphical browsers (9 kbytes). |
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http://www.atnf.csiro.au/research/images/ngc253.html
(384 words)
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| | Energy Citations Database (ECD) - Energy and Energy-Related Bibliographic Citations |
| | Availability information may be found in the Availability, Publisher, Research Organization, Resource Relation and/or Author (affiliation information) fields and/or via the "Full-text Availability" link. | | | Energy Citations Database (ECD) Document #6196110 - HCO/sup +/ in NGC 253 |
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http://www.osti.gov/energycitations/product.biblio.jsp?osti_id=6196110
(92 words)
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| | Spaceflight Now | Breaking News | X-ray view into a starburst |
| | The ellipse indicates the optical extent of NGC 253. | | | Stunning posters featuring images from the Hubble Space Telescope and world-renowned astrophotographer David Malin are now available from the Astronomy Now Store. | | | NGC 253's plume is well known since the Einstein mission. |
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http://spaceflightnow.com/news/n0101/31starburst
(907 words)
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| | Chandra :: Photo Album :: NGC 253 :: 05 Jun 01 |
| | Chandra observed NGC 253 with the Advanced CCD Imaging Spectrometer (ACIS) instrument for 3.6 hours on December 16, 1999. | | | Chandra detects a proportionally high number of suspected intermediate-size black holes – a recently discovered class of objects. | | | This Chandra X-ray image (inset) shows the central region of the starburst galaxy known as NGC 253 in comparison to the optical view. |
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http://chandra.harvard.edu/photo/2001/0012
(218 words)
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| | Astron. Astrophys. 342, 101-123 (1999) |
| | Where the source was detected during an observation block with a count rate exceeding the error filled squares are used as symbols and the errors are indicated as bars. | | | The position of the source X34 coincides with the optical center of NGC 253, X33 being located | | | For the time variable sources X12, X17 and X40 we used the maximum HRI count rates, for X21 and X36 we used the mean HRI count rate |
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http://aa.springer.de/papers/9342001/2300101/sc3.htm
(3780 words)
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| | Peculiar Gas Dynamics in the Starburst Galaxy NGC 253 |
| | --> A deep optical picture of NGC 253 (see Fig. | | | ESO optical image of the starburst galaxy NGC 253 | | | Similar features have been found in other starburst galaxies like M82, NGC 1808 and NGC 4945 and are interpreted in terms of bar-induced gas dynamics and star formation. |
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http://www.atnf.csiro.au/people/bkoribal/ngc253/n253_hi.html
(242 words)
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| | NGC 253 |
| | Photographing NGC 253 from southern France is challenging since the maximum elevation it achieves is only 20.8 degrees - average elevation during both exposures was approximately 19 degrees. | | | NGC 253 is a large magnitude 7 galaxy in the constellation of Sculptor. | | | This double stacked image improves upon the single image taken in 1997 with less graininess and improved detail. |
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http://www.astrocruise.com/ngc253.htm
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| | Caroline Lucretia Herschel |
| | She found her first object on 1783 February 26, which turned out to be an open cluster that is known today as NGC 2360. | | | Another object found in 1783 was later designated NGC 2349, but seems to be nonexistent. | | | Her second object was found on 1783 August 27 and is a galaxy with a modern designation of NGC 205. |
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http://cometography.com/biographies/herschelc.html
(1346 words)
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| | NGC 253 |
| | In the RASC's Finest N.G.C. Objects Objects list. | | | In the SAC 110 best NGC object list. | | | One supernova has been discovered in NGC 253 up to now: SN 1940E, which was discovered by Fritz Zwicky 51"W 21"S of the galaxy's nucleus, and became as bright as 14.0 mag (announced in IAUC 848). |
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http://www.seds.org/messier/xtra/ngc/n0253.html
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| | Galaxies |
| | Flare from Milky Way's Sag A* - XMM-Newton | | | NGC 4472 - ASCA (evidence for dark matter) |
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http://heasarc.gsfc.nasa.gov/docs/objects/galaxies/galaxies.html
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| | MPE Highlights 1997: Diffuse X-ray emission from nearby spiral galaxies |
| | Different emission components in the individual galaxies have been detected: point-like sources - like active galactic nuclei, X-ray binaries, supernovae (remnants) or superbubbles - and extended diffuse emission from hot interstellar medium distributed in the disk or halo. | | | The existence of a very hot component of the interstellar medium in the disk and halo of our Galaxy was predicted by Spitzer in 1956. | | | Our figures show the ROSAT PSPC contours superposed onto optical images of NGC 253 and NGC 3079. |
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http://www.mpe.mpg.de/Highlights/FB1997/h97-4-10.html
(461 words)
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| | Spiral galaxy NGC 253 |
| | For other details of photographic exposure, search technical table by AAT reference number. | | | On a very deep image the spiral structure is buried in an almost featureless halo, unremarkable except for the bulge at its southern end, which has no obvious counterpart in the brighter regions of the galaxy | | | NGC 253 is so close to us that some of the brightest stars are apparent as individuals within the spiral arms. |
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http://www.ast.cam.ac.uk/AAO/images/captions/aat023.html
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| | ESO Scientific Preprints |
| | 1404 Possible star formation in the halo of NGC 253. | | | To appear in The Astronomy and Astrophysics Review. | | | 1390 Very Large Telescope observations of the peculiar globular cluster NGC 6712. |
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http://www.eso.org/gen-fac/pubs/bin/prep-abs-sci/science-pp-2000.txt
(1027 words)
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| | The Complex X-ray Spectra of M82 and NGC 253 (ResearchIndex) |
| | The Complex X-ray Spectra of M82 and NGC 253 | | | The Complex X-ray Spectra of M82 and NGC 253 (ResearchIndex) | | | The ASCA spectra of both M82 and NGC 253 are complex with strong line emission from O, Ne, Fe, Mg, S, and Si, allowing elemental abundances to be estimated in the X-ray band for the first time in these sources. |
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http://citeseer.ist.psu.edu/110781.html
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| | NGC 253 |
| | The emission is distributed rather similar to the optical light and shows a rather regularly rotating spiral galaxy (Koribalski, Whiteoak and Houghton 1995). | | | gas distribution and velocity field of NGC 253, respectively. | | | The data were taken with three different arrays of the ATCA (12 h each). |
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http://www.atnf.csiro.au/people/bkoribal/min_lecture/node7.html
(419 words)
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| | Compact Radio Sources in NGC 253 and M82 |
| | Therefore, we believe the source variability results for NGC 253 and M82 are consistent with each other. | | | The higher frequency NGC 253 data, at resolutions as high as $0.1''$, together with scaled-array spectral-index maps at $0.4''$ to $0.6''$ resolution, reveal at least two different types of sources in the central kiloparsec of NGC 253. | | | The research described above was supported by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA, and by NSF grant AST-9120053 to UCSB. |
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http://www.aas.org/publications/baas/v25n2/aas182/abshtml/S3116.html
(319 words)
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| | NGC 253 |
| | More information about NGC 253 may be found | | | RGB: 4 x 2' each for R and G; 5 x 2' for B, binned 2 x 2. | | | NGC 253 was low in the southwest while obtaining RGB data (I needed to wait for the moon to set). |
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http://www.starrywonders.com/ngc253.html
(286 words)
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| | Roaming the Deep Sky #16 |
| | Four other NGC galaxies (55, 247, 300, and 7793) are also shown. | | | The higher an object is the less atmospheric extinction, or magnitude loss, it suffers.) NGC 253 is in the close vicinity of due south at about 1am in mid to late September, 11pm in mid to late October and around 9pm in mid to late November. | | | This group is also know as the South Polar Group since NGC 253 is located only two degrees northwest of the south galactic pole. |
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http://home.insightbb.com/~lasweb/lessons/RDS16-NGC253.htm
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| | NGC 253 |
| | Please type in the NGC number (number only, or preceded by "N" or "NGC") or the IC number preceded by "I" or "IC", or the Messier number preceded by "M". |
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http://www.seds.org/~spider/ngc/ngc.cgi?253
(40 words)
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| | Dr. Jim Ulvestad's study of NGC 253, super nova remnants and HII regions |
| | The first step in his process from idea to published paper was to get the idea. | | | Jim Ulvestad is working on his next project. | | | He is currently collaborating with another astronomer on a project in which they are studying the NGC4038/NGC4039 "Antennae" galaxies, which seem to be colliding! |
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http://www.aoc.nrao.edu/~sconrad/julvestad/JimUlvestad.htm
(394 words)
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| | X-ray astronomy |
| | Two views of NGC 253 -- a typical spiral galaxy when seen in optical wavelengths. | | | Move the mouse over the optical image to see giant outflows of hot gas as observed through the prism of X-rays. |
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http://whyfiles.org/092x_ray/index.html
(718 words)
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| | NGC 253 |
| | The linear features on the right and bottom are from rotating the frames to match either other - I left them in order to keep the images the same size for easier comparison between images. | | | This is a little deeper than the one below but exhibits a bit of "donut" syndrome around the stars due to perhaps a bit too much deconvolution. | | | same image of NGC 253 color balanced using AIPs G2V then Black color balance. |
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http://www.marcush.net/astronomy/ngc253.html
(300 words)
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| | Fabulous electric paddles in a glowing globe nebula |
| | In Ngc 3314 the condensed galaxy was stationary relative to the spiral moving in which has now cleaved the other through to the center. | | | Standard doppler shifts (red-blue) are analyzed for Ngc 1365 here | | | I am making a show that well known galaxy Ngc 1356 has had a collision with two of opposite polarities merging, so that engineering aspects of both have combined to create a new profile compositing both original's profiles in most ways intact, double the price, double the collection, so to speak. |
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http://www.cosmicastronomy.com/globe.htm
(5589 words)
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| | Astron. Astrophys. 350, 777-790 (1999) |
| | The analysis refers only to the MECS data since the quality of the LECS data statistics does not allow a more detailed study. | | | The results obtained from the spatially-resolved spectral analysis of NGC 253 are shown in Fig. | | | It should be noted, however, that analysis of ASCA data (Ptak and Griffith 1999; Matsumoto and Tsuru 1999) presumably shows that X-ray emission comes mostly from the central |
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http://aa.springer.de/papers/9350003/2300777/sc6.htm
(291 words)
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| | Mid-Infrared Spectral Mapping of NGC 253 |
| | The maps were made by scanning the long slit spectrometer across the source and reconstructing the data into a sequence of two dimensional images varying in wavelength. | | | We present 1^\prime\prime resolution mid-infrared spectral maps of the starburst galaxy NGC 253, taken with SpectroCam-10 on the Palomar 5 m telescope. |
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http://www.aas.org/publications/baas/v27n4/aas187/S049007.html
(131 words)
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| | ISO spectroscopy of OH in the starburst galaxy NGC 253 |
| | We also present ISO LWS observations CH (149 um) and H2O (179 um), and discuss their implications of these detections for models of the molecular ISM in NGC 253. | | | Using the LWS and SWS gratings, we have detected absorption in three of the four rotational lines that connect to the ground rotational state: the 119 um, the 53.3 um, and the 34.6 um doublets. | | | We present ISO SWS and LWS observations of OH in the molecular gas associated with the starburst nucleus of NGC 253. |
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http://isowww.estec.esa.nl/meetings/paris/Paris_abstracts/node217.html
(284 words)
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| | 2MASS Large Galaxy Sample |
| | It is also a remarkable study showing the decoupling of Population I and II disksùthe contrast between the visual and near-infrared windows is extreme. | | | We can further delineate the structure of NGC 253 by constructing the radial surface brightness profile and J-Ks color distribution (Figure 7). | | | The plot shown here (Figure 7) is an example of the standard product that is constructed for each source in the Large Galaxy Atlas. |
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http://spider.ipac.caltech.edu/staff/jarrett/papers/LGA/LGA_5_2.htm
(497 words)
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| | NGC 253 - Galaxy in Sculptor |
| | RAW to TIFF conversion, frame calibrations, alignment and stacking, Digital Development, Adaptive Richardson_Lucy deconvolution, scaling and JPEG conversion with ImagesPlus. | | | This image was the first astronomical photo taken with the new Canon 10D Digital SLR camera. | | | NGC 253 lies at a distance of 8 million light years. |
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http://www.machunter.org/hap_ngc253.html
(131 words)
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| | [No title] |
| | The Kinematics of the Ionized and Molecular Hydrogen in the Starburst Galaxy NGC 253 | | | Detection of the SO mbox {J_{N} =} 1_0 -> 0_1 Rotational Transition in NGC 253: Comparison of the Molecular Abundances among Extragalaxies | | | The Distribution of the Dense Clouds in the Starburst Nucleus of NGC 253 |
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http://www.columbia.edu/~fms5/w346.html
(496 words)
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| | IngentaConnect The ortho- to para- ratio of H2 in the starburst of NGC 253 |
| | The rotation curves of 1-0 S(1) and Brgamma suggest that the ionized gas is tracing a kinetic system different from that of the molecular gas in NGC 253, particularly away from the nucleus. | | | We have been able to measure four H2 lines across the circumnuclear starburst, from which we estimate the ortho- to para- ratio of excited H2 to be =~2. | | | The ortho- to para- ratio of H2 in the starburst of NGC 253 |
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http://www.ingentaconnect.com/content/bsc/mnr/1998/00000297/00000002/art01525
(336 words)
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| | APOD: November 2, 1996 - Spiral Galaxy NGC 253 Almost Sideways |
| | NGC 253 is considered a "starburst" galaxy because of high star formation rates and dense dust clouds in its nucleus. | | | Each day a different image or photograph of our fascinating universe is featured, along with a brief explanation written by a professional astronomer. | | | NGC 253 appears visually as one of the brightest spirals on the sky, and is easily visible in southern hemisphere with a good pair of binoculars. |
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http://antwrp.gsfc.nasa.gov/apod/ap961102.html
(137 words)
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| | Jul 2000 - X-ray color image of the galaxy NGC253 |
| | Crosses show the positions of the point sources detected with ROSAT. | | | NGC 253 is featured by strong star formation in the central region combined with intensive X-ray emission. | | | This X-ray image of the galaxy NGC 253 seen edge-on was taken with the PSPC camera of the ROSAT observatory. |
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http://wave.xray.mpe.mpg.de/rosat/calendar/2000/jul
(236 words)
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| | Jahrbuch-CD der MPG 2003 - The collimated wind in NGC 253 |
| | The outflow is tilted with respect to the disk, possibly suggesting the inhomogeneous nature of the interstellar medium in which the starburst takes place. | | | It is closely related to the hot plasma observed in soft X-rays: filamentary H-2 features are found at the edges of the hot plasma. | | | Near-infrared Fabry-Perot imaging has revealed H-2 emission extended to about 130 pc from the disk of NGC 253. |
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http://www.mpg.de/forschungsergebnisse/wissVeroeffentlichungen/archivListenJahrbuch/2003/26/publZIM153.html
(172 words)
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| | [No title] |
| | I will infer the nature of the starburst in NGC 253 by comparing the results from the Mauna Kea telescopes with observations made at far-IR and radio wavelengths." | | | I will discuss a detailed case study of PDRs in the nearby starburst NGC 253, concentrating on observations made with UKIRT and the JCMT. |
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http://www.jach.hawaii.edu/Seminars/abstracts/970718_harrison.html
(83 words)
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| | MPE Jahresbericht 2000 - IV / MPE Annual Report 2000 - IV |
| | Schinnerer, E., A. Eckart and L.J. Tacconi: Distribution and Kinematics of the Circumnuclear Molecular Gas in the Seyfert 1 Galaxy NGC 3227. | | | Anders, L.E. Tacconi-Garman and N. Thatte: Stellar Dynamics and the Implications on the Merger Evolution in NGC 6240. | | | Spoon, H.W.W., J. Koornneef, A.F.M. Moorwood, D. Lutz and A.G.G.M. Tielens: Mid-infrared spectroscopy of NGC 4945. |
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http://www.mpe.mpg.de/JB2000/publications.html
(11123 words)
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| | Simulation of NGC 253 |
| | As a first attempt to simulate this source, the SIS0 spectrum from a 6' region (composite diffuse + point source flux) was fit with a power-law plus gaussian lines model, providing a good fit (see figure). | | | NGC 253 is a starburst galaxy containing diffuse, extended thermal emission and multiple point sources. |
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http://lheawww.gsfc.nasa.gov/~ptak/trace2/old/n253.html
(116 words)
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| | Universe Today - What's Up This Week - November 14 - November 20, 2005 |
| | Echoing it less than a fistwidth south of Beta Cetii is the equally grand NGC 253. | | | While this wonderful galaxy is around one quarter the size of the M31 and dimmer at magnitude 7.0, it is no less lacking in terms of observational structure. | | | This magnitude 5.0 spiral galaxy and all of its richest are easily viewed with the smallest of binoculars to the largest of telescopes. |
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http://www.universetoday.com/am/publish/whatsup_nov14_2005.html
(1892 words)
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| | Estimating Starburst Supernova Rates Using OSSE Observations of M82 and NGC 253 (ResearchIndex) |
| | Monte Carlo simulations of randomly occurring supernova events in NGC 253 and M82 were performed to evaluate the significance of our upper limit to the 0.847 and1.238 MeV 56 Co gamma-ray line fluxes on the supernova rate from these two galaxies. | | | A set of observations of NGC 253 and M82 by OSSE is suggested in order to maximize the chances... | | | Abstract: We have used the OSSE observations of the starburst galaxies NGC 253 and M82 to obtain upper limits to the Type Ia and Ib supernova rates in these galaxies. |
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http://citeseer.ist.psu.edu/347972.html
(280 words)
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| | Hubble Heritage |
| | The Hubble Space Telescope (HST) data of NGC 253 provide a detailed view of the central 5,800 light years. | | | In the image to the left, the HST view is overlaid on a photograph (by David Malin) taken at the Anglo-Australian Observatory. | | | Note that all the views of NGC 253 on this page are oriented with |
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http://heritage.stsci.edu/1998/42/supplemental2.html
(224 words)
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| | APOD: December 9, 1998 - NGC 253: The Sculptor Galaxy |
| | NGC 253 is the largest member of the | | | The dense dark dust accompanies a high star formation rate, giving NGC 253 the designation of | | | Explanation: NGC 253 is not only one of the brightest spiral galaxies visible, it is also one of the dustiest. |
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http://antwrp.gsfc.nasa.gov/apod/ap981209.html
(116 words)
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| | SPACE.com -- Building Bigger Black Holes: How Middleweights May Join Forces |
| | In an interview, Weaver said the core of NGC 253, like many galaxies in which a lot of star formation is going on, is loaded with stars, gas and dust. | | | "In NGC 253, Chandra may have found a causal connection." | | | The galaxy, called NGC 253, is known as a starburst galaxy. |
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http://www.space.com/scienceastronomy/astronomy/aas_midblackhole_010605.html
(1380 words)
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