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16 September, 2014

Astronomers Release Most Detailed Catalogue Ever Made of the Visible Milky Way

A new catalogue of the visible part of the northern part of our home galaxy, the Milky Way, includes no fewer than 219 million stars. Geert Barentsen of the University of Hertfordshire led a team who assembled the catalogue in a ten year programme using the Isaac Newton Telescope (INT) on La Palma in the Canary Islands. Their work appears today in the journal Monthly Notices of the Royal Astronomical Society.

From dark sky sites on Earth, the Milky Way appears as a glowing band stretching across the sky. To astronomers, it is the disk of our own galaxy, a system stretching across 100,000 light-years, seen edge-on from our vantage point orbiting the Sun. The disk contains the majority of the stars in the galaxy, including the Sun, and the densest concentrations of dust and gas.

The unaided human eye struggles to distinguish individual objects in this crowded region of the sky, but the 2.5-m mirror of the INT enabled the scientists to resolve and chart 219 million separate stars. The INT programme charted all the stars brighter than 20th magnitude – or almost 1 million times fainter than can be seen with the human eye.

Using the catalogue, the scientists have put together an extraordinarily detailed map of the disk of the galaxy that shows how the density of stars varies, giving them a new and vivid insight into the structure of this vast system of stars, gas and dust.

The image included here, a cut-out from a stellar density map mined directly from the released catalogue, illustrates the new view obtained.  The Turner-like brush strokes of dust shadows would grace the wall of any art gallery. Maps like these also stand as useful tests of new-generation models for the Milky Way.

A density map of part of the Milky Way disk, constructed from IPHAS data. The scales show galactic latitude and longitude, coordinates that relate to the position of the centre of the galaxy. The mapped data are the counts of stars brighter than 20th magnitude detected in Sloan i, the longer (redder) wavelength broad band of the survey. Although this is just a small section of the full map, it portrays in exquisite detail the complex patterns of obscuration due to interstellar dust. This image contains 600 × 2400 independent data points, each of which represents the star count within 1 × 1 square arcminute cells (1 arcminute is 1/60th of a degree). At the level of the original exposed images, each cell is itself made up of 32,000 pixels. The typical effective angular resolution of the data is close to 1 arcsecond (1/3600th of a degree or about 10 original image pixels). The section shown features the edge of the Sagittarius spiral arm (near longitude 60 degrees) and the Cygnus-X molecular cloud complex (at around 80 degrees longitude). Both of these appear as regions of reduced star counts due to the obscuring effect of higher dust concentrations. Credit: The stellar density map has been produced by Hywel Farnhill as part of his PhD project at the University of Hertfordshire. Copper colour scale image of the density map: Linear count scale [ labelled | borderless ], square-root count scale [ labelled | borderless ].


The production of the catalogue, IPHAS DR2 (the second release from the survey programme The INT Photometric H-alpha Survey of the Northern Galactic Plane  or IPHAS), is an example of modern astronomy's exploitation of 'big data' – it contains information on the 219 million detected objects, each of which is summarised in 99 attributes.

With this catalogue release, the team are offering the world community free access to measurements taken through two broad band filters capturing light at the red end of the visible spectrum, and in a narrowband capturing the brightest hydrogen emission line, H-alpha. The inclusion of H-alpha also enables exquisite imaging of the nebulae (glowing clouds of gas) found in greatest number within the disk of the Milky Way. The stellar density map illustrated here is derived from the longest (reddest) wavelength band in which the darkening effect of the dust is moderated in a way that brings out more of its structural detail, compared to maps built at shorter (bluer) wavelengths.

Contacts:

Dr Geert Barentsen
University of Hertfordshire
Tel: +44 (0)17 0728 4603
Mob: +44 (0)75 4700 3148
g.barentsenherts.ac.uk

Prof Janet Drew
University of Hertfordshire
Tel: +44 (0)1707 286576
Mob: +44 (0)7758 918823
j.drewherts.ac.uk

Further information:

The new work appears in Barentsen et al, 2014, "The second data release of the INT Photometric Hα Survey of the Northern Galactic Plane (IPHAS DR2)", Monthly Notices of the Royal Astronomical Society, 444, 3230, published by Oxford University Press. A preprint version is available on the arXiv server.

The catalogue is accessible in queryable form via the VizieR service at the Centre de Données astronomiques de Strasbourg. The processed IPHAS images it is derived from are also publically available. The preparation of the catalogue was funded by the Science and Technology Facilities Council.

IPHAS is the acronym standing for "The INT Photometric H-alpha Survey of the Northern Galactic Plane" (see the IPHAS survey website). IPHAS, in combination with its follow-on sister survey UVEX, imaging the Milky Way using complementary blue filters, has used the Wide Field Camera on the INT in observing campaigns stretching over more than 500 allocated nights since August 2003. Together with another survey, VPHAS+, now in progress on a telescope in Chile, these ambitious observational programmes are collectively known as the European Galactic Plane Surveys (EGAPS). They are exploiting modern high-resolution CCD imaging technology and the growth in computing power to map the entire disk of our galaxy in visible light and at high angular resolution for the first time.

Recently reported results derived from IPHAS survey data include a 3-D reconstruction of the distribution of dust across the Milky Way's disk (Sale et al. 2014, MNRAS, 443, 2907) and the discovery of 159 new planetary nebulae (Sabin et al. 2014, MNRAS, 443, 3388).



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Last modified: 16 September 2014