See also rise and set times. Small Magellanic Cloud, field of NGC 330 Aims.We search for the effects of metallicity on B and Be stars in theSmall and Large Magellanic Clouds (SMC and LMC) and in the Milky Way(MW), by extending our previous analysis of B and Be star populations inthe LMC to the SMC. – Coordinates: RA: … I have therefore looked at the range of magnitudes in different wavelength ranges in several references, and at the visual magnitude estimates in Steve Gottlieb's visual examination of the NGC/IC objects. The New General Catalog (NGC) is a listing of nearly 8,000 non-stellar objects, such as star clusters, nebulae, and galaxies, compiled by J.L.E. Visual magnitude and apparent dimension (arc min unless indicated as arc sec) Remarks Apparent size 0.85 by 0.35 arcmin. Its current altitude is 42° above the horizon. NGC 5350 Group: 13h53m24s +40°22' Canes Venatici: This group is positioned near a 6.5 magnitude star and has a bright spiral galaxy, NGC 5471 less than a half degree to the northeast. A variable star periodically triples its light output. For example, Sirius has a magnitude of –1.46, while the brightest planet, Venus, can reach magnitude –4.9 at its brightest. A good object for f/2 Fastar imaging. – Object type: Open cluster. IV. NGC 6804 is above the horizon from Greenwich, United Kingdom . This spiral galaxy was discovered by Messier in 1780. NGC 6993 - The object is declared as "not found" in the RNGC and so the type is "-" in Sinnott's book. 3. NGC 7331 is the brightest member of the NGC 7331 Group of galaxies. All structured data from the file and property namespaces is available under the Creative Commons CC0 License; all unstructured text is available under the Creative Commons Attribution-ShareAlike License; additional terms may apply. ... previous HST imagingdata. This list of stars is based on the 'NGC 2000.0' version of the catalog, which lists the stars in its errata, supplemented with data on each individual star from the VizieR database. NGC 7331 was discovered in 1784 by the famous astronomer, William Herschel. Caroline’s Cluster. Messier 46 (NGC 2437) is an open cluster with an apparent magnitude of 6.5. NGC 5248: m = 10.97. Messier object M31 (NGC 224), also known as the Andromeda Galaxy, is a spiral galaxy located in the constellation Andromeda in the Local Group of galaxies. – Magnitude: +3 – Distance: About 1,321 light years – Other designations: C 1104-584, Caldwell 91, Melotte 103, Football Cluster, Wishing Well Cluster. But actually NGC 6993 is a bright Sc galaxy (13.8 mag) in Capricornus.. IC 252 - Sinnott does not identify the object (type "blank"), but actually this is a pretty bright double galaxy with a total magnitude of 15.5 mag, located in Cetus. Physical Information: The asterism consists of five 14th to 15th magnitude stars arranged in a north-south oval, and a few much fainter stars that Cooper could not have seen; so the NGC object is basically just the five brighter stars. Dreyer over 100 years ago. Objects are sorted by catalog number, starting with Messier list, then NGC, IC and so on. "Best" objects are marked in bold. September 9, 2015 Messier 103 (M103) is an open star cluster located in the northern constellation Cassiopeia. The Messier objects are a set of 110 astronomical objects catalogued by the French astronomer Charles Messier in his Catalogue des Nébuleuses et des Amas d'Étoiles ("Catalogue of Nebulae and Star Clusters"). The cluster has an apparent magnitude of 7.1. If unchecked, all the objects will be displayed irrespective of brightness. The cluster lies at an approximate distance of 4,000 light years from Earth. The Double Cluster, or Caldwell 14, is the name for two open clusters – NGC 869 and NGC 884 – located close together in Perseus constellation.Also known as h Persei and χ Persei (h and Chi Persei), the clusters both lie at an approximate distance of 7,600 light … Stars. It is 178' in size. The resultant colour-magnitude diagrams indicate that thecluster is an intermediate-age object of 1.4 Gyr. Typical of reflection nebulae, they appear bluish resulting from light reflection from hot young stars by the interstellar dust, with darker regions dividing the three NGC objects. Only 35' to the southwest is the dauntingly dim object called the Bubble Nebula (NGC 7635), an even fainter ring of gas, whose brightest section abuts a 9th-magnitude star. – Constellation: Canis Major. The 1,165 NGC objects in the NexStar 60/76/80/102/114/4/130 GT hand control database, including Dreyer's descriptions. Globular clusters with composite color-magnitude diagrams, such as NGC1851, NGC 2808, and Fornax 3, might have formed by mergers. NGC 5897 is a globular cluster in Libra with a low surface brightness, making it a more challenging object than its magnitude (8.5) would suggest. The Interactive NGC Catalog Online by Hartmut Frommert. Some of the populations are found to belocated beyond the Perseus arm and may be the part of the Norma-Cygnus(outer) arm. Messier 29 is too faint to be spotted by the naked eye, but can be seen in binoculars. For reference, the … Effects of metallicity, star-formation conditions, and evolution in B and Be stars. II. M31 is best viewed during winter, is magnitude 4.5 *, and can be viewed with naked eye. Pre-main sequence stars in open clusters. It issuggested that each of these objects had two parent clusters, one with ared horizontal branch and another with a blue horizontal branch. See also rise and set times. NGC 5774-75: 14h54m00s +03°33' Virgo Files are available under licenses specified on their description page. Together with M65 and NGC 3628, the three galaxies are referred to as the Leo Triplet or the Trio in Leo. 6.31 times brighter. Objects without magnitude (i.e. Its designation in the New General Catalogue is NGC 581. Variables in the Field of NGC 1245 The Survey for Transiting Extrasolar Planets in Stellar Systems (STEPSS)project is a search for planetary transits in open clusters. Available Resources for NGC 2608 - Spiral Galaxy Messier 47 (M47) Messier 47 (NGC 2422) is an open cluster in Puppis. By how much does the apparent magnitude change? In thispaper we analyze the STEPSS observations of the open cluster NGC 1245 todetermine the variable-star content of the cluster. Above, a 9 arcmin wide DSS image centered on NGC 2218 NGC 2219 2. Given its B magnitude of 13.2, NGC 2608 is visible with the help of a telescope havng an aperture of 10 inches (250mm) or more. Answers: 1. I. For reference, the full moon is 30' (arc minutes) in size. Given its visual magnitude of 12, NGC 6804 is visible with the help of a telescope havng an aperture of 8 inches (200mm) or more. This page was last edited on 8 February 2011, at 20:40. M66 lies at an estimated distance of 35 million light years. 2. The Equinox 2000 coordinates are RA= 11h 20.2m, Dec= +12° 59´. Some objects originally thought to be deep sky objects and listed in the NGC have been subsequently shown to be ordinary stars, so their inclusion in the catalog is now considered erroneous. The cluster lies at a distance of 10,000 light years from Earth and has an apparent magnitude of 7.4. 3. This is the interactive NGC (and IC, and Messier) catalog at SEDS, based on the famous NGC 2000.0 by R.W. This grouping is positioned half a degree northeast of the great nebula. Sinnott of Sky Publishing Corp., who also created the electronic version used by this online service (thanks to Sky Publishing for permitting us this kind of use). It spans about 30,000 light years, lies about 68 million light years from Earth and can be seen with a small telescope in the constellation of Ursa Major. The RASC's Finest N.G.C. The list is limited to declination -60°. NGC 2608 is below the horizon from Greenwich, United Kingdom [ change ]. The First 30 NGC objects By Paul Markov, October 1999. Messier 66 or M66 (also designated NGC 3627) is a spiral galaxywith an apparent visual magnitude of 8.9 and an angular diameter is 8x2.5 arc-minutes. Messier 46. It lies about 5,400 light years from Earth in the direction of Puppis constellation. The absolute magnitude of the variablewas determined from the period-luminosity (P-L) relation for Galacticδ Scuti stars and from theoretical modeling of the observed B,V,Ilight curves with nonlinear pulsation models. 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