Lockman Hole

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Chandra X-ray Observatory mosaic of the X-ray sources in the Lockman Hole. Color code: Energy (red 0.4-2.0 keV, green 2-8 keV, blue 4-8 keV). Image is about 50 arcmin per side. Credit: X-ray: NASA/CXC/U. Wisconsin/A.Barger et al.; Illustrations: NASA/CXC/M.Weiss. Lockman Hole.jpg
Chandra X-ray Observatory mosaic of the X-ray sources in the Lockman Hole. Color code: Energy (red 0.4–2.0 keV, green 2–8 keV, blue 4–8 keV). Image is about 50 arcmin per side. Credit: X-ray: NASA/CXC/U. Wisconsin/A.Barger et al.; Illustrations: NASA/CXC/M.Weiss.

The Lockman Hole is an area of the sky in which minimal amounts of neutral hydrogen gas are observed from the perspective of Earth. The Lockman Hole is a relatively clear window on distant objects, which makes it an attractive area of the sky for observational astronomy surveys. It is located near the pointer stars of the Big Dipper in the constellation Ursa Major and is ~15 square degrees in size. [1] [2]

Contents

The Lockman Hole is named after its discoverer, astronomer F. Jay Lockman.

Location

The Lockman Hole is located at about RA 10h 45m, Dec. +58° and is defined by a region of low neutral hydrogen gas and dust column density. [3] Column density is a commonly used measure in astronomy for the quantity of a given chemical element or molecule in a certain direction. In this region, the typical column density of neutral hydrogen is NH = 0.6 x 1020 cm−2. [4] This column density is moderately lower than typical values near the galactic poles, where NH 1020 cm−2, and H I column densities of NH > 1021 cm−2 are common at low galactic latitudes and towards H I clouds. [5]

The region around B1950.0 RA 10h 45m Dec 57° 20′ has a minimum NH of 4.5 x 1019 cm−2. [3] There is a diffuse cloud covering half of the field. [3] [6]

The Lockman Hole East is a subregion of the Lockman Hole centered at J2000.0 RA 10h 52m Dec +57°. [7]

The Lockman Hole North-west (LHNW) is a region that appears about as wide as the moon centered at J2000.0 RA 10h 34m Dec +57° 40′., [8] [9] with a column density of NH = 5.72 x 1019 cm−2. [5]

Hydrogen gas absorption and emission

Clouds of neutral hydrogen are ubiquitous in the Milky Way galaxy, and effectively absorb photons that are energetic enough to ionize hydrogen, which requires an energy of 13.6 electron volts (in the extreme ultraviolet range). Even the relatively small amounts of hydrogen in the Lockman Hole absorb most radiation at and just above energies of 13.6 electron volts, but even so it transmits extreme ultraviolet and soft x-ray radiation from extragalactic objects to a greater degree than other areas of the sky.

Neutral hydrogen is also associated with diffuse emission at infrared wavelengths that can confuse observations of faint infrared sources.

Observations

The relatively clear field of view offered by the Lockman Hole has allowed its use to view extremely distant regions of the universe. Observations by the Spectral and Photometric Imaging Receiver (SPIRE) instrument aboard the Herschel Space Telescope of the Lockman Hole have imaged thousands of extremely distant galaxies that appear as they did 10–12 billion years ago. [10]

This field of view also contains hundreds of astronomical X-ray sources, some of them supermassive black holes. The Chandra X-ray Observatory and ROSAT have been used to study X-ray sources from the Lockman Hole. [4] Some 75 X-ray sources are observed with the PSPC of ROSAT. [4]

Detailed X-ray spectral analysis has been performed on 123 X-ray sources in the Lockman Hole using XMM-Newton. [11]

The diffuse X-ray background (XRB) has also been studied in the area. [12] [13]

Active galactic nuclei have also been studied in the area, for example MBC2005. [11]

See also

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References

  1. ↑ "Is the Big Dipper scooping dark matter?". CSMonitor.com. 2011-02-18. Retrieved 2011-12-10.
  2. ↑ "Lockman Hole". Encyclopedia of Science. Retrieved 2011-12-10.
  3. 1 2 3 Lockman FJ, Jahoda K, McCammon D (Mar 1986). "The structure of galactic HI in directions of low total column density". Astrophys. J. 302 (3): 432–49. Bibcode:1986ApJ...302..432L. doi:10.1086/164002. hdl: 2060/19850019473 . S2CID   118595586.
  4. 1 2 3 Hasinger G, Burg R, Giacconi R, Hartner G, Schmidt M, Trumper J, Zamorani G; Burg; Giacconi; Hartner; Schmidt; Trumper; Zamorani (Aug 1993). "A Deep X-Ray Survey in the Lockman-Hole and the Soft X-Ray N-Log". Astron. Astrophys. 275 (1): 1–15. Bibcode:1993A&A...275....1H.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  5. 1 2 Dickey JM, Lockman FJ (1990). "H I in the Galaxy". Annu. Rev. Astron. Astrophys. 28 (1): 215–61. Bibcode:1990ARA&A..28..215D. doi:10.1146/annurev.aa.28.090190.001243.
  6. ↑ Schlegel DJ, Finkbeiner P, Davis M (Jun 1998). "Maps of dust infrared emission for use in estimation of reddening and cosmic microwave background radiation foregrounds". Astrophys. J. 500 (2): 525–53. arXiv: astro-ph/9710327 . Bibcode:1998ApJ...500..525S. doi:10.1086/305772. S2CID   59512299.
  7. ↑ "SHADES: SCUBA Half Degree Extragalactic Survey" . Retrieved 2011-12-10.
  8. ↑ "Shape of Universe seen during adolescent years". Spaceflight Now. 2003-03-23. Retrieved 2011-12-10.
  9. ↑ Yang Y, Mushotzky RF, Steffen AT, Barger AJ, Cowie LL (Oct 2004). "The Chandra Large Area Synoptic X-Ray Survey (CLASXS) of the Lockman Hole-Northwest: The X-Ray Catalog". Astron. J. 128 (4): 1501–23. arXiv: astro-ph/0409087 . Bibcode:2004AJ....128.1501Y. doi:10.1086/423996. S2CID   8216340.
  10. ↑ "Star-forming galaxies like grains of sand". Archived from the original on 2011-06-14. Retrieved 2010-06-01.
  11. 1 2 Mateos S, Barcons X, Carrera FJ, Ceballos MT, Hasinger G, Lehmann I, Fabian AC, Streblyanska A (Dec 2005). "XMM-Newton observations of the Lockman Hole: search for AGNs". Astron. Astrophys. 444 (1): 79–99. arXiv: astro-ph/0506718 . Bibcode:2005A&A...444...79M. doi:10.1051/0004-6361:20052881. S2CID   211409.
  12. ↑ Mather, J. C.; Cheng, E. S.; Cottingham, D. A.; Eplee, R. E. Jr.; Fixsen, D. J.; Hewagama, T.; Isaacman, R. B.; Jensen, K. A.; Meyer, S. S.; Noerdlinger, P. D.; Read, S. M.; Rosen, L. P.; Shafer, R. A.; Wright, E. L.; Bennett, C. L.; Boggess, N. W.; Hauser, M. G.; Kelsall, T.; Moseley, S. H. Jr.; Silverberg, R. F.; Smoot, G. F.; Weiss, R.; Wilkinson, D. T. (January 1994). "Measurement of the cosmic microwave background spectrum by the COBE FIRAS instrument". The Astrophysical Journal. 420 (2): 439–44. Bibcode:1994ApJ...420..439M. doi: 10.1086/173574 .
  13. ↑ Mather; et al. (1990). "A preliminary measurement of the cosmic microwave background spectrum by the Cosmic Background Explorer (COBE) satellite". Astrophys. J. 354: L37. Bibcode:1990ApJ...354L..37M. doi: 10.1086/185717 .

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