HEIC: Hubble Sees a Galaxy Hit a Bull's-Eye (NGC 922)

[bystander]

Hubble Sees a Galaxy Hit a Bull's-Eye
ESA/HEIC | NASA/STScI | 2012 Dec 06

Click to view full size image 1 or image 2

Bright pink nebulae almost completely encircle a spiral galaxy in this NASA/ESA Hubble Space Telescope image of NGC 922. The ring structure and the galaxy’s distorted spiral shape result from a smaller galaxy scoring a cosmic bullseye, hitting the centre of NGC 922 some 330 million years ago.

In Hubble’s image, NGC 922 clearly reveals itself not to be a normal spiral galaxy. The spiral arms are disrupted, a stream of stars extends out towards the top of the image, and a bright ring of nebulae encircles the core. Observing with NASA’s Chandra X-ray Observatory reveals more chaos in the form of ultraluminous X-ray sources dotted around the galaxy.

NGC 922’s current unusual form is a result of a cosmic bullseye millions of years ago. A smaller galaxy, catalogued as 2MASXI J0224301-244443, plunged right through the heart of NGC 922 and shot out the other side. In wide-field views of the NGC 922, the small interloper can be still be seen shooting away from the scene of the crash.

As the small galaxy passed through the middle of NGC 922, it set up ripples that disrupted the clouds of gas, and triggered the formation of new stars whose radiation then lit up the remaining gas. The bright pink colour of the resulting nebulae is a characteristic sign of this process, and it is caused by excited hydrogen gas (the dominant element in interstellar gas clouds). This process of excitation and emission of light by gases is similar to that in neon signs.

In theory, if two galaxies are aligned just right, with the small one passing through the centre of the larger one, the ring of nebulae should form a perfect circle, but more often the two galaxies are slightly off kilter, leading to a circle that, like this one, is noticeably brighter on one side than the other.

These objects, called collisional ring galaxies, are relatively rare in our cosmic neighbourhood. Although galaxy collisions and mergers are commonplace, the precise alignment and ratio of sizes necessary to form a ring like this is not, and the ring-like phenomenon is also thought to be relatively short-lived.

The chances of seeing one of these galaxies nearby is therefore quite low. Despite the immense number of galaxies in the Universe, this is one of only a handful known in our cosmic neighbourhood (the Cartwheel Galaxy, see potw1036a, being the most famous example). Observations of the more distant Universe (where we see further into the past) show that these rings were more common in the past, however.

Hubble’s image of NGC 922 consists of a series of exposures taken in visible light with Hubble’s Wide Field Camera 3, and in visible and near-infrared light with the Wide Field and Planetary Camera 2. In the overlay, shown in blue, are X-ray sources dotted around the galaxy, spotted with the NASA Chandra X-ray Observatory.

Credit: Optical (NASA/ESA/Hubble); X-ray (NASA/CXC/SAO)

A Galaxy Takes a Bullet to the Heart
Slate Blogs | Bad Astronomy | 2012 Dec 06

Pink Galactic Smackdown Results in Cosmic Bullseye
Universe Today | John Williams | 2012 Dec 06

[Ann]

Wow, that's a really fascinating galaxy that I hadn't heard about, and it is a very beautiful picture! The HEIC link says that it's a five-filter image! Fantastic! One filter is generally red at 621 nm, one is redshifted Ha at 665 nm and one is infrared at 814 nm. I was beginning to despair when I read this and started wondering if they had constructed this image from various shades of red (fifty shades of red?), but then I saw that they had used a green filter as well and an honest-to-God blue one, too. Fantastic!

And this is indeed a great galaxy! According to my software its U-B color is -0.40, which is ultraviolet indeed and a confirmation of all the hot OB stars that ionize all those red emission nebulae. The B-V of the galaxy is +0.33, which is really quite blue for a galaxy. And according to the PGC catalog in my software (and this catalog isn't totally reliable) this galaxy is one and a half times as bright as the Milky Way. Galaxies so large and so blue are unusual, but I guess that's what you get when a gas-rich galaxy has a head-on collision.

Ann

[bystander]

NGC 922: Searching for the Best Black Hole Recipe
NASA | SAO | Chandra X-ray Observatory | 2012 Dec 06

In this holiday season of home cooking and carefully-honed recipes, some astronomers are asking: what is the best mix of ingredients for stars to make the largest number of plump black holes?

They are tackling this problem by studying the number of black holes in galaxies with different compositions. One of these galaxies, the ring galaxy NGC 922, is seen in this composite image containing X-rays from NASA's Chandra X-ray Observatory (red) and optical data from the Hubble Space Telescope (appearing as pink, yellow and blue).

NGC 922 was formed by the collision between two galaxies - one seen in this image and another located outside the field of view. This collision triggered the formation of new stars in the shape of a ring. Some of these were massive stars that evolved and collapsed to form black holes.

Most of the bright X-ray sources in Chandra's image of NGC 922 are black holes pulling material in from the winds of massive companion stars. Seven of these are what astronomers classify as "ultraluminous X-ray sources" (ULXs). These are thought to contain stellar-mass black holes that are at least ten times more massive than the sun, which places them in the upper range for this class of black hole. They are a different class from the supermassive black holes found at the centers of galaxies, which are millions to billions of times the mass of the sun.

Theoretical work suggests that the most massive stellar-mass black holes should form in environments containing a relatively small fraction of elements heavier than hydrogen and helium, called 'metals' by astronomers. In massive stars, the processes that drive matter away from the stars in stellar winds work less efficiently if the fraction of metals is smaller. Thus, stars with fewer of these metals among their ingredients should lose less of their mass through winds as they evolve. A consequence of this reduced mass loss is that a larger proportion of massive stars will collapse to form black holes when their nuclear fuel is exhausted. This theory appeared to be supported by the detection of a large number (12) of ULXs in the Cartwheel galaxy, where stars typically contain only about 30% of the metals found in the sun.

To test this theory, scientists studied NGC 922, which contains about the same fraction of metals as the sun, meaning that this galaxy is about three times richer in metals than the Cartwheel galaxy. Perhaps surprisingly, the number of ULXs found in NGC 922 is comparable to the number seen in the Cartwheel galaxy. Rather, the ULX tally appears to depend only on the rate at which stars are forming in the two galaxies, not on the fraction of metals they contain.

One explanation for these results is that the theory predicting the most massive stellar-mass black holes should form in metal poor conditions is incorrect. Another explanation is that the metal fraction in the Cartwheel galaxy is not low enough to have a clear effect on the production of unusually massive stellar-mass black holes, and therefore will not cause an enhancement in the number of ULXs. Recent models incorporating the evolution of stars suggest that a clear enhancement in the number of ULXs might only be seen when the metal fraction falls below about 15%. Astronomers are investigating this possibility by observing galaxies with extremely low metal fractions using Chandra. The number of ULXs is being compared with the number found in galaxies with higher metal content. The results of this work will be published in a future paper.

Image Credits: X-ray (NASA/CXC/SAO/A.Prestwich et al); Optical (NASA/STScI)

Chandra Observations of the Collisional Ring Galaxy NGC 922 - A. H. Prestwich et al

• Astrophysical Journal 747(2) 150 (2012 Mar 10) DOI: 10.1088/0004-637X/747/2/150
  arXiv.org > astro-ph > arXiv:1212.1124 > 05 Dec 2012