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2 edition of Hubble Space Telescope observations of globular clusters in M31 I found in the catalog.

Hubble Space Telescope observations of globular clusters in M31 I

Hubble Space Telescope observations of globular clusters in M31 I

color-magnitude diagrams, horizontal branch metallicity dependence, and the distance to M31

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Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English

    Subjects:
  • Globular clusters.,
  • Spaceborne astronomy.,
  • Metallicity.,
  • Image analysis.,
  • Stellar magnitude.,
  • Stellar spectra.,
  • Stellar color.,
  • Brightness.

  • Edition Notes

    StatementEdward A. Ajhar ... [et al.].
    Series[NASA contractor report] -- NASA CR-201958.
    ContributionsAjhar, Edward A., United States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL15452341M

    One of the driving forces behind this behavior is thought to be gravity: more massive globulars manage to grab more gas and dust, which can then be transformed into new stars. IC is a somewhat special case. After ejecting most of their mass and exhausting much of their hydrogen fuel, the stars appear brilliant blue. It has long been believed that all the stars within a globular cluster form at the about same time, a property which can be used to determine the cluster's age. References: Ajhar, E. Loose OB associations.

    This ensures that the photometric quality of the reductions are comparable, and we conclude that our internal photometric errors are at most as high as those quoted by Ajahr et al. This cluster is roughly six times further than the Virgo cluster, hence uncertainties introduced by peculiar local velocities have a much smaller effect on our estimate of the Hubble constant. The final M vs. Adjustments made to the HB magnitudes of the metal rich clusters are discussed in the full paper. The first set of stars gobble up most of the gas, then as they die millions of years later they eject the gas.

    The majority of the stars in the image are yellow-white, like our Sun. Bootstrapping our way to the Coma cluster leads to an estimate of Mpc for the Hubble constant. That's because the original gas cloud of which the clusters were created was also not rotating rapidly, Richer said. Because of the HST optical aberration, however, accurate photometry of individual stars for a Colour-Magnitude Diagram has not been possible so far, and only surface brightness profiles could be obtained.


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Hubble Space Telescope observations of globular clusters in M31 I book

In the first case, this second nucleus may be a remainder of a possibly violent dynamical encountering event in the earlier history of the Local Group. The stars in Omega Centauri are between 10 billion and 12 billion years old.

Hubble revisits a globular cluster's age

This is a preview of subscription content, log in to check access. C, Sparks, W. M22 was a notable find not only for its early discovery, but also for the ages of the stars within it. The cluster lies about 16 light-years from Earth. Some globular clusters, such as Messier 13 M13 in the constellation Herculescan be seen with the naked eye.

Because HB magnitudes for metal-rich clusters as determined above are actually contaminated by red RGB stars and, moreover, the ridge point so adopted can hardly be taken to represent the luminosity level of the HB at the instability strip a part from the problems of evolution within the strip which should be somehow taken into accountwe adopted a procedure a priori to correct the observed V for this problem Ajhar et al.

The zero-point, crucial to absolute age determinations, is also affected by an additional error due to the residual uncertainties in the HST photometric zero-points mag, at least. Lucas, F. Globular clusters are big balls of old stars that orbit around their host galaxy.

While it is well established that M31 is about times further away than the Large Magellanic Cloud LMCthe absolute value of this measure is still uncertain, and in current sources, usually given between 2. In astronomer Harlow Shapley, studying Cepheids, a certain kind of variable star within each cluster, noted that these stars shine at a predictable brightness depending on distance from the receiver.

The best known and most readily observed satellite galaxies are M32 and M This object is what's called a planetary nebula, which is what remains after a star has died and puffed out its outer gaseous layers.

At the same time, the telescope gave hints as to why M87 which is embedded in the same region has more star clusters than what would be expected.

The majority of the stars in the image are yellow-white, like our Sun. Building on Shapley's research, Edwin Hubble found globular clusters that were even more distant — as much as 10 times farther — and that lay beyond the Milky Way, in other galaxies.

Using the data listed in Table 1 and plotted in Figure 3, 1 error-barwe have computed the best fitting solution to the available points taking into account the size of the errors in both axes.

Because he was not aware of the two Cepheid classes, his distance was incorrect by a factor of more than two, though. Evidence suggests, however, that Omega Centauri has at least two populations of stars with different ages.

However, only Hartwig realized its significance. Simulations show that the smaller galaxy passed through the disk of the Andromeda Galaxy along the latter's polar axis.

Recent research with the Hubble Space Telescope revealed that the original population is more centered in the globular cluster, while newer stars slowly diffuse outward. At this stage, they emit much of their light at ultraviolet wavelengths.

The optimal PSF has been determined from the analysis of the brightest uncrowded stars independently in both frames in each color.

Whitmore, R. IC is a somewhat special case. It faded to mag 16 in February This result is of course strongly dependent on various assumptions more or less explicitly made during the procedure and must be checked in detail.Title: Wide-Field Hubble Space Telescope Observations of the Globular Cluster System in NGC Authors: Thomas H.

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Puzia, Maurizio Paolillo, We present a comprehensive high spatial-resolution imaging study of globular clusters (GCs) in NGC, the central giant elliptical cD galaxy in the Fornax galaxy cluster, conducted with HST/ACS Cited by: Figure: CMDs of the 7 globular clusters observed in M31 with HST.

Table 1: Relevant data for the 7 globular clusters observed in M31 with HST. Using the data listed in Table 1 (and plotted in Figure 3, 1 error-bar), we have computed the best fitting solution to the available points taking into account the size of the errors in both axes.

*Description*: Hubble Space Telescope has captured a view of a globular cluster called G1, a large, bright ball of light in the center of the photograph consisting of at leastold stars. G1, also known as Mayall II, orbits the Andromeda galaxy (M31), the nearest major spiral galaxy to our Milky Way.

The first known globular cluster, now called M 22, was discovered in by Abraham Ihle, a German amateur astronomer. However, given the small aperture of early telescopes, individual stars within a globular cluster were not resolved until Charles Messier observed M 4 in The first eight globular clusters discovered are shown in the table.

The NASA/ESA Hubble Space Telescope snapped this panoramic view of a colourful assortment of stars residing in the crowded core of a giant star cluster.

The image reveals a small region inside the massive globular cluster Omega Centauri, which boasts nearly 10 million stars.

Space Telescope Science Institute, San Martin Drive, Baltimore, MDUSA. Abstract: Hubble Space Telescope observations of over a thousand globular clusters in the central region of M87 have been made using the WFPC The limiting magnitude in V is 26 mag, more than two magnitudes beyond the turnover of the luminosity function.