The surprising turbulent past of metal rich halo of Messier 104 1

The Surprising Turbulent Past Of Metal Rich Halo Of Messier 104

The surprising turbulent past of metal rich halo of Messier 104 represents Messier 104, a lenticular galaxy located 28 million light years away in the constellation Virgo. Messier 104 is a lenticular galaxy located 28 million light years away in the constellation Virgo. Now it has a new chapter in its history.

An expanded halo of metal-rich stars, a sign of the expected metal-poor stars seen under the influence of other galaxies. This Hubble image shows Messier 104. Image from NASA / ESA / Hubble Heritage Team.

Astronomer and team member of the Space Telescope Science Institute, Drs. Paul Goudfreuse said: “Also known as the Sombrero galaxy, Messier 104 has always been a kind of strange galaxy, which makes it interesting.”

He added: “Hubble’s measure of metallicity (that is, the abundance of heavy elements in the stars) is another indication that Messier 104 has much to teach us about the assembly and evolution of galaxies. Dr. of the Space Telescope Science Institute. Roger Cohen stated:

Observing the hat’s halo is changing the accepted understanding of galaxy makeup and metallurgy over our heads. Astronomers, discussing Hubble’s new data, turned to sophisticated computer models to suggest explanations about the extreme inversion of traditional galactic theory.

The results suggest an equally surprising possibility of major mergers in the galaxy’s past, although Messier 104’s majestic structure is not evidence of recent disruption. “The absence of metal-poor stars was a big surprise,” said Dr. Gaudfreuise, and the abundance of metal-rich stars only added to the mystery.

On the left is an image of Messier 104 that includes a very bright portion of the greeting outside its bright disk and bump. Hubble represented two areas in the halo (one of which is represented by a white box). The images are captured in the right zoom to show the level of detail of the Hubble.

Orange Box, a small subset of the Hubble scene, which includes countless Halo stars. The density increases near the disk of the galaxy (blue box below). Each frame consists of a bright circular cluster of stars, many of which are found in the halo of the galaxy.

The halo of Messier 104 had more metal-rich stars than expected, but even more strange was the absence of older and metal-poor stars that are commonly found in manifestations of massive galaxies. However, many spherical clusters have metal-poor stars.

A possible explanation of the macular characteristics of Messier 104 is that it is the product of a fusion of massive galaxies thousands of millions of years ago, although the smooth appearance of the galaxy’s discs and halos showed no signs of a disruption. so big.

Astronomers in the halo of a galaxy expect to find previous generations of stars with less massive elements than the crowded star cities present on the galaxy’s main disk. The elements are created through the process of the stellar life cycle, and the more time the stars spend in the galaxy this cycle.

The more gases rich in elements and highly metallic stars are formed from that gas. These small, highly metallic stars are usually found on the main disk of the galaxy, where stellar populations are dense, or so conventional wisdom says.

The facts that complain is the presence of many clusters of spherical stars older and poor in metals. These older and metal-poor stars are expected to finally come out of their clusters and become part of the normal star halo, but this process seems to have been inefficient in Messier 104.

Astronomers compared their results with recent computer simulations to see what could be the origin of such unexpected measurements of metals in the galaxy’s halo. The results also challenged expectations, indicating that the unaffected Messier 104 had suffered events or mergers that occurred billions of years earlier.

Unlike our galaxy, the Milky Way, which is believed to have swallowed many smaller satellite galaxies in billions of years in the so-called “nominal” accumulation, a larger accumulation is a fusion of two or more equally massive galaxies that were enriched in later generations. They are high-metal stars.

Satellite galaxies have only fewer metal stars that were largely hydrogen and helium from the Big Bang. The heavier elements would be cooked in stellar interiors through nucleosynthesis and incorporated into the stars of the later generation.

This process was not effective in dwarf galaxies, such as those in our Milky Way, and was dominant in larger and more evolved galaxies. The results of Messier 104 are surprising because its smooth disc shows no signs of interruption.

In comparison, many conflicting galaxies, such as iconic antenna galaxies, derive their names from the distortions of their spiral arms due to their tidal contact forces. Mergers of similar massive galaxies generally encompass large, smooth elliptical galaxies, which have been billions of years with widespread disclosure.

But Messier 104 has never been compatible with the traditional definition of a spiral or elliptical galaxy. It is somewhere in the middle of a hybrid. The study was published in the Astrophysical Journal.

Detection of Messier 104: M104 is easily found at 11 degrees, approximately one phisfer, west of Alpha Virginis (Spica). With excellent conditions from a dark sky site, it can be seen in the telescope as a small patch of light in the shape of an eye. With binoculars as small as 3 3 in the aperture.

It takes on a galactic signature and reveals its dark plane starting at about 4.5 ″ in the aperture. Ability to collect more light, reveal more beautiful Galaxy Hat! As always, galaxies prefer dark points in the sky and good viewing conditions.

What you’re looking at: Sombrero, also known as M104, is the largest galaxy in the nearby Virgo cluster about 28 million light years from Earth. This great view of the famous Sombrero Galaxy Observatory was created using NASA’s Lunar X-ray Observatory, Hubble Space Telescope, and Spitzer Space Telescope.

The main figure shows the combined image of three telescopes, while the three inserted images show different views of the observatory. Chandra’s x-ray image (in blue) shows hot gas in the galaxy and point sources that are a mixture of objects inside the hat, as well as quasars in the background.

Chandra’s observations show that the diffuse X-ray emission extends 60,000 light years from the center of the Sombrero. (The galaxy itself spans 50,000 light years.) Scientists believe that this extended X-ray glow may be the result of a galaxy wind, driven primarily by supernovae that form its bulk and disk. It has exploded within.

The Hubble optical image (green) shows a lump of stars partially blocked by a dust rim, as this spiral galaxy is viewed from the side. The dusty edge itself appears brighter in Spitzer’s infrared image, which also suggests that the hat is the central bulge of the stars. Like “Diamonds in the Hat”.

The circular clusters are all bundles and are part of the makeup of the M104. Images for the Survey Hubble Space Telescope Advanced Camera are used to conduct a new photometric study of spherical groups (GC) at M104 in the Somstero galaxy.

The main focus of our study is the GCS characteristic distribution function of the linear form [size distribution function (SDF)]. We measure ready for 652 groups with a dynamic fit of King and Wilson model decorated with dot functions.

SDF is remarkably measured for all types of other large galaxies, adding strong support for the view that it is a ‘universal’ feature of the GC system. We used the Hat and Milky Way data and the Baumgardt and Kroupa (2007) formation model to develop a more general interpretation of SDF for GCB.

We propose that the size of the SDFs that we observe today for GCFs is strongly influenced by the rapid loss of mass during their star formation phase, which is combined with the group-to-group stochastic difference in star formation efficiency (SFE ) and their initial sizes are..

We found that the observed SDF size can be estimated using a simple model in which the protoprotector clouds had a size of 0.9 of 0.1 pc and an SFE of 0.3 ± 0.07. States Valliam E. Harris. The colors and brightness of the M104 clusters show a clearly defined classic bimodal appearance.

The blue color sequence exhibits a large scale / metallic relationship, with the brightness of Z following the scale of the abundance of heavy elements. L0.3 is similar to that found in most massive elliptical galaxies. A quantitative self-enrichment model provides a good first-order match with initial SFE data and the size of the protocols required to explain SDF.

We also discuss various forms of the GC fundamental plane of structural parameters and note that its useful evidence can extend to galaxies beyond the local cluster. M104 clusters closely resemble the Milky Way and other nearby systems in terms of test volumes such as integrated surface density and bond energy.

But, like our own galaxy, spherical clusters are not hidden within that terrible halo. We used the CTI4M telescope to perform a complete and kinematically unbiased study of M104 (NGC 4594; galaxy hat) for the planet’s nebula (ie stars) up to 16 kpc.

We present 294 planetary positions and the monochromatic magnitude [O III] Lambda 5007, and use the luminosity function of the observed planetary nebula (PNLF) to measure a distance of 8.9 +/- 0.6 centimeters for the galaxy.

“We used the distance from PN104 to M104 to compare their brightness to the brightest galaxies in the Virgo galaxy, discovering that if M104 were in the Virgo cluster, it would be the third brightest galaxy.

We combined the distance to the PNLF and the speeds corrected for the Virgo drop to calculate the Hubble constant/ mpc. We also used PNLF distances for the NGC 1023 group, the Leo group, the Virgo group, and the Fornax group, to obtain the Hubble constant, which was true for the female baby.

The H_0_ values for M104, NGC 1023 groups, Virgo groups, and Fornax groups are in excellent agreement, suggesting that PNLF distances and Schechter’s linear decay model provide a self-sufficient representation of Hubble span and Virgo decay.

History: Messier 104 was not included in Messier’s originally published catalog. However, Charles Messier folded it by hand in his personal copy on May 11, 1781, calling him “a much-loved nebula.” It was Camille Flemrian who discovered that her position was Herschel HI43 matches the Galaxy Hat (NGC 4594), and was added to Messier’s official list in 1921.

Pierre Mekin also mentions this article as his discovery: May 11 from 1781, I discovered a nebula above the crow [Corvus], in which I couldn’t find any stars. It is a light light and it is difficult to detect if the micrometer cables are illuminated.

I have compared [his position] with this day and the next with Speka on the Virgin and its correct origin as 187d 9 ″ 42 its and his southern proclamation 10d 24 ″ 49 the [Messier’s handwritten note has the same position] Does not appear in the consens des temps.

William Herschel found the object independently on May 9, 1784, but his son John would be the first to note that there was something different about it: There is a dim diffuse oval light about it, and I am almost certain there is a gap or stratum deep that separates the nucleus and the normal mass of the nebula from the light above.

There is definitely no confusion. There is a faint diffuse oval light about it, and I am almost certain that the light from above (from the south) is an interval dark or stratum that separates the nucleus and the normal mass of the nebula.

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