انتخاب نام (ساگیتاریوس *Sagittarius A) به این صورت ناشی از دلیلهای تاریخی است: در سال ۱۹۵۴،جان دی کراوس به همراه «هسین-چینگ کو» و «شان مت» منابع رادیویی را؛ که با تلسکوپ رادیوییدانشگاه ایالتی اوهایو با فرکانس ۲۵۰ مگاهرتز شناسایی و فهرست کرده بودند، منابع آن فرکانسها را بر اساس بخشهایی از صورت فلکی مرتب کردند و حرف اختصاص داده شده به آنها به دلخواه و (A) نشان دهندهٔ درخشانترین منبع رادیویی در صورت فلکی بود. نشان ستاره (*) هم به دلیل «هیجانانگیز» بودن کشف آن در نظر گرفته میشده و در فیزیک اتمی، نامگذاری اتمهای در حالت برانگیخته نیز با یک ستاره نشان داده میشود.
نتیجهٔ مشاهدات چندین ستارهٔ در حال گردش به دور کمان ای*؛ به ویژه ستاره اس۲، برای تعیین جرم و حد بالای شعاع این جسم مورد استفاده قرار گرفتهاست. بر اساس جرم و محدودیت شعاع دقیق فزاینده، اخترشناسان به این نتیجه رسیدهاند که کمان ای* سیاهچالهٔ کلانجرم مرکزی کهکشان راه شیری است. مقدار فعلی جرم آن برابر ۴٫۱۵۴ میلیون (± ۰٫۰۱۴) جرم خورشیدی است.
در ۱۲ مهٔ ۲۰۲۲، اخترشناسان با استفاده از تلسکوپ افق رویداد، تصویری از کمان ای* را منتشر کردند که با استفاده از دادههای مشاهدات رادیویی در آوریل ۲۰۱۷، تهیه شده بود، که سیاهچاله بودن این شی را تأیید میکرد. این دومین تصویر تأیید شده از یک سیاهچاله، پس از سیاهچالهٔ کلانجرم مسیه ۸۷ در سال ۲۰۱۹ است.
نیوستار نخستین نماهای متمرکز از سیاهچالهٔ کلانجرم مرکزی کهکشان راه شیری را در: پیش از وضوح (بالا)، واضحترین (وسط) و پس از وضوح (پایین) با پرتوهای ایکس پرانرژی ثبت کردهاست.
در مقالهای که در ۳۱ اکتبر ۲۰۱۸ منتشر شد، کشف شواهد قطعی مبنی بر اینکه کمان ای* یک سیاهچاله است، اعلام شد. اخترشناسان با استفاده از تداخل سنجگرانش GRAVITY و چهار تلسکوپ تلسکوپ بسیار بزرگ (VLT) برای ایجاد یک تلسکوپ مجازی به قطر ۱۳۰ متر، تودههایی از گاز را شناسایی کردند که با حدود ۳۰ درصد سرعت نور حرکت میکردند.انتشار از الکترونهای بسیار پرانرژی بسیار نزدیک به سیاهچاله به صورت سه شعله درخشان برجسته قابل مشاهده بود. اینها دقیقاً با پیشبینیهای نظری مربوط به نقاط داغی که نزدیک به یک سیاهچاله با جرم چهار میلیون برابر جرم خورشیدی میچرخند مطابقت دارند. تصور میشود که شرارهها از فعل و انفعالات مغناطیسی در گاز بسیار داغی که در مداری بسیار نزدیک به کمان ای* میچرخد، سرچشمه میگیرند.
مدارهای بررسی شدهٔ ۶ ستاره به دور سیاهچاله کلان پرجرم کمان ای* در مرکز کهکشان راه شیری
ستارگان مداری پیرامون کمان ای* آنگونه که در سال ۲۰۱۸ مشاهده شدند.
ستارگان مداری پیرامون کمان ای* برابر مشاهدات ثبتشده در سال ۲۰۲۱.
ستارگانی به دور کمان اِی* در مدار نزدیک به آن وجود دارند که در جمع به عنوان "ستارههای S" شناخته میشوند. این ستارگان عمدتاً در طول موجهای باند K فروسرخ مشاهده میشوند، زیرا غبار کیهانی بهشدت دید را در طولموجهای مرئی محدود میسازد. وضعیت این میدان به سرعت در حال تغییر است - در سال ۲۰۱۱، مدارهای برجستهترین ستارگانی که در آن زمان شناخته شده بودند در نمودار ترسیم شده، که مقایسهای بین مدار آنها و مدارهای مختلف در منظومه شمسی را نشان میدهد.
مقایسه نشان میدهد که از آن زمان ستارهٔ اس۲ بیشتر از دیگر ستارگان مداری به سیاهچاله نزدیک شدهاست.
داشتن سرعتهای بالا و نزدیک شدن به سیاهچالههای عظیم باعث میشود که این ستارگان برای ایجاد محدودیتهایی در ابعاد فیزیکی کمان A* و همچنین مشاهدهٔ اثرات مرتبط با نسبیت عام مانند تغییر دور چشمی مدارشان مفید باشند. یک نظارت پیگیر برای احتمال نزدیک شدن ستارگان به افق رویداد؛ به اندازهای نزدیک که درهم گسیخته شود، انجام میشود، اما انتظار نمیرود هیچیک از این ستارهها به این سرنوشت دچار شوند: توزیع آماری مشاهده شدهٔ صفحات مدارهای ستارگان S، اسپین کمان A* را به کمتر از ۱۰ درصد حداکثر مقدار نظری آن محدود میکند.
تا سال ۲۰۲۰، ستارهٔ «اس۴۷۱۴» رکورددار نزدیکترین نزدیکی به کمان A* بودهاست، در حدود ۱۲٫۶ واحد نجومی (۱٫۸۸ میلیارد کیلومتر)، تقریباً به اندازهٔ نزدیکی زحل به خورشید، که با حدود ۸ درصد سرعت نور حرکت میکند. این ارقام ارائه شده تقریبی هستند، عدم قطعیتهای رسمی ۹٫۳±۱۲٫۶ واحد نجومی و ۲۳۹۲۸±۸۸۴۰ کیلومتر بر ثانیه است. دوره مداری آن ۱۲ سال است، اما خروج از مرکز فوقالعاده ۰٫۹۸۵ به آن نزدیک شدن نزدیک و سرعت بالا میدهد.
The object is a bright and very compact astronomical radio source. The name Sagittarius A* follows from historical reasons. In 1954,John D. Kraus, Hsien-Ching Ko, and Sean Matt listed the radio sources they identified with the Ohio State University radio telescope at 250 MHz. The sources were arranged by constellation and the letter assigned to them was arbitrary, with A denoting the brightest radio source within the constellation. The asterisk* is because its discovery was considered "exciting", in parallel with the nomenclature for excited state atoms which are denoted with an asterisk (e.g. the excited state of Helium would be He*). The asterisk was assigned in 1982 by Robert L. Brown, who understood that the strongest radio emission from the center of the galaxy appeared to be due to a compact nonthermal radio object.
The observations of several stars orbiting Sagittarius A*, particularly star S2, have been used to determine the mass and upper limits on the radius of the object. Based on mass and increasingly precise radius limits, astronomers have concluded that Sagittarius A* must be the Milky Way's central supermassive black hole. The current value of its mass is 4.154±0.014 million solar masses.
Detection of an unusually bright X-ray flare from Sgr A*
On May 12, 2022, the first image of Sagittarius A* was released by the Event Horizon Telescope Collaboration. The image, which is based on radio interferometer data taken in 2017, confirms that the object contains a black hole. This is the second image of a black hole. This image took five years of calculations to process. The data were collected by eight radio observatories at six geographical sites. Radio images are produced from data by aperture synthesis, usually from night long observations of stable sources. The radio emission from Sgr A* varies on the order of minutes, complicating the analysis.
In 2019, measurements made with the High-resolution Airborne Wideband Camera-Plus (HAWC+) mounted in the SOFIA aircraft revealed that magnetic fields cause the surrounding ring of gas and dust, temperatures of which range from −280 to 17,500 °F (99.8 to 9,977.6 K; −173.3 to 9,704.4 °C), to flow into an orbit around Sagittarius A*, keeping black hole emissions low.
Karl Jansky, considered a father of radio astronomy, discovered in April 1933 that a radio signal was coming from a location in the direction of the constellation of Sagittarius, towards the center of the Milky Way. The radio source later became known as Sagittarius A. His observations did not extend quite as far south as we now know to be the Galactic Center. Observations by Jack Piddington and Harry Minnett using the CSIRO radio telescope at Potts Hill Reservoir, in Sydney discovered a discrete and bright "Sagittarius-Scorpius" radio source, which after further observation with the 80-foot (24-metre) CSIRO radio telescope at Dover Heights was identified in a letter to Nature as the probable Galactic Center.
ALMA observations of molecular-hydrogen-rich gas clouds, with the area around Sagittarius A* circled
Later observations showed that Sagittarius A actually consists of several overlapping sub-components; a bright and very compact component, Sgr A*, was discovered on February 13 and 15, 1974, by astronomers Bruce Balick and Robert Brown using the baseline interferometer of the National Radio Astronomy Observatory. The name Sgr A* was coined by Brown in a 1982 paper because the radio source was "exciting", and excited states of atoms are denoted with asterisks.
Since the 1980s, it has been evident that the central component of Sgr A* is likely a black hole. In 1994, infrared and submillimetre spectroscopy studies by a Berkeley team involving Nobel LaureateCharles H. Townes and future Nobel Prize Winner Reinhard Genzel showed that the mass of Sgr A* was tightly concentrated and of the order 3 million Suns.
On October 16, 2002, an international team led by Reinhard Genzel at the Max Planck Institute for Extraterrestrial Physics reported the observation of the motion of the star S2 near Sagittarius A* throughout a period of ten years. According to the team's analysis, the data ruled out the possibility that Sgr A* contains a cluster of dark stellar objects or a mass of degenerate fermions, strengthening the evidence for a massive black hole. The observations of S2 used near-infrared (NIR) interferometry (in the Ks-band, i.e. 2.1 μm) because of reduced interstellar extinction in this band. SiO masers were used to align NIR images with radio observations, as they can be observed in both NIR and radio bands. The rapid motion of S2 (and other nearby stars) easily stood out against slower-moving stars along the line-of-sight so these could be subtracted from the images.
Dusty cloud G2 passes the supermassive black hole at the center of the Milky Way
The VLBI radio observations of Sagittarius A* could also be aligned centrally with the NIR images, so the focus of S2's elliptical orbit was found to coincide with the position of Sagittarius A*. From examining the Keplerian orbit of S2, they determined the mass of Sagittarius A* to be 4.1±0.6 millionsolar masses, confined in a volume with a radius no more than 17 light-hours (120 AU [18 billionkm; 11 billion mi]). Later observations of the star S14 showed the mass of the object to be about 4.1 million solar masses within a volume with radius no larger than 6.25 light-hours (45 AU [6.7 billion km; 4.2 billion mi]). S175 passed within a similar distance. For comparison, the Schwarzschild radius is 0.08 AU (12 million km; 7.4 million mi). They also determined the distance from Earth to the Galactic Center (the rotational center of the Milky Way), which is important in calibrating astronomical distance scales, as 8,000 ± 600 parsecs (30,000 ± 2,000 light-years). In November 2004, a team of astronomers reported the discovery of a potential intermediate-mass black hole, referred to as GCIRS 13E, orbiting 3 light-years from Sagittarius A*. This black hole of 1,300 solar masses is within a cluster of seven stars. This observation may add support to the idea that supermassive black holes grow by absorbing nearby smaller black holes and stars.
After monitoring stellar orbits around Sagittarius A* for 16 years, Gillessen et al. estimated the object's mass at 4.31±0.38 million solar masses. The result was announced in 2008 and published in The Astrophysical Journal in 2009.Reinhard Genzel, team leader of the research, said the study has delivered "what is now considered to be the best empirical evidence that supermassive black holes do really exist. The stellar orbits in the Galactic Center show that the central mass concentration of four million solar masses must be a black hole, beyond any reasonable doubt."
On January 5, 2015, NASA reported observing an X-ray flare 400 times brighter than usual, a record-breaker, from Sgr A*. The unusual event may have been caused by the breaking apart of an asteroid falling into the black hole or by the entanglement of magnetic field lines within gas flowing into Sgr A*, according to astronomers.
On 13 May 2019, astronomers using the Keck Observatory witnessed a sudden brightening of Sgr A*, which became 75 times brighter than usual, suggesting that the supermassive black hole may have encountered another object.
NuSTAR has captured these first, focused views of the supermassive black hole at the heart of the Milky Way in high-energy X-rays
In a paper published on October 31, 2018, the discovery of conclusive evidence that Sagittarius A* is a black hole was announced. Using the GRAVITYinterferometer and the four telescopes of the Very Large Telescope (VLT) to create a virtual telescope 130 metres (430 feet) in diameter, astronomers detected clumps of gas moving at about 30% of the speed of light. Emission from highly energetic electrons very close to the black hole was visible as three prominent bright flares. These exactly match theoretical predictions for hot spots orbiting close to a black hole of four million solar masses. The flares are thought to originate from magnetic interactions in the very hot gas orbiting very close to Sagittarius A*.
In July 2018, it was reported that S2 orbiting Sgr A* had been recorded at 7,650 km/s (17.1 million mph), or 2.55% the speed of light, leading up to the pericenter approach, in May 2018, at about 120 AU (18 billionkm; 11 billion mi) (approximately 1,400 Schwarzschild radii) from Sgr A*. At that close distance to the black hole, Einstein's theory of general relativity (GR) predicts that S2 would show a discernible gravitational redshift in addition to the usual velocity redshift; the gravitational redshift was detected, in agreement with the GR prediction within the 10 percent measurement precision.
Assuming that general relativity is still a valid description of gravity near the event horizon, the Sagittarius A* radio emissions are not centered on the black hole, but arise from a bright spot in the region around the black hole, close to the event horizon, possibly in the accretion disc, or a relativistic jet of material ejected from the disc. If the apparent position of Sagittarius A* were exactly centered on the black hole, it would be possible to see it magnified beyond its size, because of gravitational lensing of the black hole. According to general relativity, this would result in a ring-like structure, which has a diameter about 5.2 times the black hole's Schwarzschild radius (10 μas). For a black hole of around 4 million solar masses, this corresponds to a size of approximately 52 μas, which is consistent with the observed overall size of about 50 μas, the size (apparent diameter) of the black hole Sgr A* itself being 20 μas.
Recent lower resolution observations revealed that the radio source of Sagittarius A* is symmetrical. Simulations of alternative theories of gravity depict results that may be difficult to distinguish from GR. However, a 2018 paper predicts an image of Sagittarius A* that is in agreement with recent observations; in particular, it explains the small angular size and the symmetrical morphology of the source.
The mass of Sagittarius A* has been estimated in two different ways:
Two groups—in Germany and the U.S.—monitored the orbits of individual stars very near to the black hole and used Kepler's laws to infer the enclosed mass. The German group found a mass of 4.31±0.38 million solar masses, whereas the American group found 4.1±0.6 million solar masses. Given that this mass is confined inside a 44-million-kilometre-diameter sphere, this yields a density ten times higher than previous estimates.
More recently, measurement of the proper motions of a sample of several thousand stars within approximately one parsec from the black hole, combined with a statistical technique, has yielded both an estimate of the black hole's mass at 3.6+0.2 −0.4×106M☉, plus a distributed mass in the central parsec amounting to (1±0.5)×106M☉. The latter is thought to be composed of stars and stellar remnants.
Ultimately, what is seen is not the black hole itself, but observations that are consistent only if there is a black hole present near Sgr A*. In the case of such a black hole, the observed radio and infrared energy emanates from gas and dust heated to millions of degrees while falling into the black hole. The black hole itself is thought to emit only Hawking radiation at a negligible temperature, on the order of 10−14kelvin.
In July 2019, astronomers reported finding a star, S5-HVS1, traveling 1,755 km/s (3.93 million mph) or 0.006 c. The star is in the Grus (or Crane) constellation in the southern sky, and about 29,000 light-years from Earth, and may have been propelled out of the Milky Waygalaxy after interacting with Sagittarius A*.
Inferred orbits of 6 stars around supermassive black hole candidate Sagittarius A* at the Milky Way's center
Stars moving around Sagittarius A* as seen in 2018
Stars moving around Sagittarius A* as seen in 2021
There are a number of stars in close orbit around Sagittarius A*, which are collectively known as "S stars". These stars are observed primarily in K band infrared wavelengths, as interstellar dust drastically limits visibility in visible wavelengths. This is a rapidly changing field—in 2011, the orbits of the most prominent stars then known were plotted in the diagram at left, showing a comparison between their orbits and various orbits in the solar system. Since then, S62 has been found to approach even more closely than those stars.
The high velocities and close approaches to the supermassive black hole makes these stars useful to establish limits on the physical dimensions of Sagittarius A*, as well as to observe general-relativity associated effects like periapse shift of their orbits. An active watch is maintained for the possibility of stars approaching the event horizon close enough to be disrupted, but none of these stars are expected to suffer that fate. The observed distribution of the planes of the orbits of the S stars limits the spin of Sagittarius A* to less than 10% of its theoretical maximum value.
As of 2020[update], S4714 is the current record holder of closest approach to Sagittarius A*, at about 12.6 AU (1.88 billion km), almost as close as Saturn gets to the Sun, traveling at about 8% of the speed of light. These figures given are approximate, the formal uncertainties being 12.6±9.3 AU and 23,928±8,840 km/s. Its orbital period is 12 years, but an extreme eccentricity of 0.985 gives it the close approach and high velocity.
An excerpt from a table of this cluster (see Sagittarius A* cluster), featuring the most prominent members. In the below table, id1 is the star's name in the Gillessen catalog and id2 in the catalog of the University of California, Los Angeles. a, e, i, Ω and ω are standard orbital elements, with a measured in arcseconds. Tp is the epoch of pericenter passage, P is the orbital period in years and Kmag is the infrared K-bandapparent magnitude of the star. q and v are the pericenter distance in AU and pericenter speed in percent of the speed of light.
First noticed as something unusual in images of the center of the Milky Way in 2002, the gas cloud G2, which has a mass about three times that of Earth, was confirmed to be likely on a course taking it into the accretion zone of Sgr A* in a paper published in Nature in 2012. Predictions of its orbit suggested it would make its closest approach to the black hole (a perinigricon) in early 2014, when the cloud was at a distance of just over 3,000 times the radius of the event horizon (or ≈260 AU, 36 light-hours) from the black hole. G2 has been observed to be disrupting since 2009, and was predicted by some to be completely destroyed by the encounter, which could have led to a significant brightening of X-ray and other emission from the black hole. Other astronomers suggested the gas cloud could be hiding a dim star, or a binary star merger product, which would hold it together against the tidal forces of Sgr A*, allowing the ensemble to pass by without any effect. In addition to the tidal effects on the cloud itself, it was proposed in May 2013 that, prior to its perinigricon, G2 might experience multiple close encounters with members of the black-hole and neutron-star populations thought to orbit near the Galactic Center, offering some insight to the region surrounding the supermassive black hole at the center of the Milky Way.
The average rate of accretion onto Sgr A* is unusually small for a black hole of its mass and is only detectable because it is so close to Earth. It was thought that the passage of G2 in 2013 might offer astronomers the chance to learn much more about how material accretes onto supermassive black holes. Several astronomical facilities observed this closest approach, with observations confirmed with Chandra, XMM, VLA, INTEGRAL, Swift, Fermi and requested at VLT and Keck.
As the cloud approached the black hole, Dr. Daryl Haggard said, "It's exciting to have something that feels more like an experiment", and hoped that the interaction would produce effects that would provide new information and insights.
Nothing was observed during and after the closest approach of the cloud to the black hole, which was described as a lack of "fireworks" and a "flop". Astronomers from the UCLA Galactic Center Group published observations obtained on March 19 and 20, 2014, concluding that G2 was still intact (in contrast to predictions for a simple gas cloud hypothesis) and that the cloud was likely to have a central star.
An analysis published on July 21, 2014, based on observations by the ESO's Very Large Telescope in Chile, concluded alternatively that the cloud, rather than being isolated, might be a dense clump within a continuous but thinner stream of matter, and would act as a constant breeze on the disk of matter orbiting the black hole, rather than sudden gusts that would have caused high brightness as they hit, as originally expected. Supporting this hypothesis, G1, a cloud that passed near the black hole 13 years ago, had an orbit almost identical to G2, consistent with both clouds, and a gas tail thought to be trailing G2, all being denser clumps within a large single gas stream.
Professor Andrea Ghez et al. suggested in 2014 that G2 is not a gas cloud but rather a pair of binary stars that had been orbiting the black hole in tandem and merged into an extremely large star.
Artist impression of the accretion of gas cloud G2 onto Sgr A*. Credit: ESO
This simulation shows a gas cloud, discovered in 2011, as it passes close to the supermassive black hole at the center of the Milky Way
This video sequence shows the motion of the dusty cloud G2 as it closes in on, and then passes, the supermassive black hole at the center of the Milky Way.