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Serpens CaputSerpens Cauda
Abbreviation Ser
Genitive Serpentis
Pronunciation /ˈsɜrpɨnz/,
genitive /sərˈpɛntɨs/
Symbolism the Snake
Right ascension Serpens Caput: 15h 10.4m to 16h 22.5m
Serpens Cauda: 17h 16.9m to 18h 58.3m
Declination Serpens Caput: 25.66° to −03.72°
Serpens Cauda: 06.42° to −16.14°
Family Hercules
Area Serpens Caput: 428 sq. deg.
Serpens Cauda: 208 sq. deg.
Total: 637 sq. deg. (23rd)
Main stars 11
Stars with planets 15
Stars brighter than 3.00m 1
Stars within 10.00 pc (32.62 ly) 2
Brightest star α Ser (Unukalhai) (2.63m)
Nearest star GJ 1224
(24.60 ly, 7.54 pc)
Messier objects 2
Serpens Caput:
Corona Borealis

Serpens Cauda:
Visible at latitudes between +80° and −80°.
Best visible at 21:00 (9 p.m.) during the month of July.

Serpens ("the Serpent", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the "Serpent-Bearer". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.

The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known, Arp 220, the prototypical ultraluminous infrared galaxy, and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.

Part of the Milky Way passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape, and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an HII region.


Serpens held by Ophiuchus, as depicted in Urania's Mirror, a set of constellation cards published in London c. 1825. Above the tail of the serpent is the now-obsolete constellation Taurus Poniatovii while below it is Scutum.

In Greek Mythology, Serpens represents a snake held by the healer Asclepius. Represented in the sky by the constellation Ophiuchus, Asclepius was known for killing a snake that was resurrected because a different snake had placed a certain herb on it before its "death". Serpens is depicted as either winding around Ophiuchus in the night sky or simply passing through him, although the precise reason for either of these is unknown. In some ancient atlases, the constellations Serpens and Ophiuchus were depicted as two separate constellations, although in most they were shown as a single constellation. Back in this time, there were no official constellation boundaries, so when depicted separately, their bodies were not intertwined with each other. With the establishment of modern constellation boundaries, Serpens is split into two halves by the snake-bearer.[1]

In Chinese astronomy, most of the stars of Serpens represented part of a wall surrounding a marketplace, known as Tianshi, which was in Ophiuchus and part of Hercules. Serpens also contains a few Chinese constellations. Two stars in the tail represented part of Shilou, the tower with the market office. Another star in the tail represented Liesi, jewel shops. One star in the head (Mu Serpentis) marked Tianru, the crown prince's wet nurse, or sometimes rain.[1]

There were two "serpent" constellations in Babylonian astronomy, known as Mušḫuššu and Bašmu. It appears that Mušḫuššu was depicted as a hybrid of a dragon, a lion and a bird, and loosely corresponded to Hydra. Bašmu was a horned serpent (c.f. Ningishzida) and loosely corresponds to the Ὄφις constellation of Eudoxus of Cnidus on which the Ὄφις (Serpens) of Ptolemy is based.[2]


Serpens is the only one of the 88 modern constellations to be split into two disconnected regions in the sky: Serpens Caput (the head) and Serpens Cauda (the tail). The constellation is also unusual in that it depends on another constellation for context; specifically, it is being held by the Serpent Bearer Ophiuchus.[1]

Serpens Caput is bordered by Libra to the south, Virgo and Boötes to the east, Corona Borealis to the north, and Ophiuchus and Hercules to the west; Serpens Cauda is bordered by Sagittarius to the south, Scutum and Aquila to the east, and Ophiuchus to the north and west. Covering 636.9 square degrees total, it ranks 23rd of the 88 constellations in size. It appears prominently in the both the northern and southern skies during the Northern Hemisphere's summer.[3] Its main asterism consists of 11 stars, and 108 stars in total are brighter than magnitude 6.5.[3]

Serpens Caput's boundaries, as set by Eugène Delporte in 1930, are defined by a 15-sided polygon, while Serpens Cauda's are defined by a 25-sided polygon. In the equatorial coordinate system, the right ascension coordinates of Serpens Caput's borders lie between 15h 10.4m and 16h 22.5m, while the declination coordinates are between 25.66° and −03.72°. Serpens Cauda's boundaries lie between right ascensions of 17h 16.9m and 18h 58.3m and declinations of 06.42° and −16.14°.[4] The International Astronomical Union (IAU) adopted the three-letter abbreviation "Ser" for the constellation in 1922.[5]

Notable features[edit]

The constellation Serpens (Caput) as it can be seen by the naked eye


Head stars[edit]

The brightest star in Serpens and marking its heart, Alpha Serpentis, or Unukalhai, is a red giant of spectral type K2III located approximately 22.68 parsecs (74.0 ly) away. With a visual magnitude of 2.63,[6] it can easily be seen with the naked eye even in areas with substantial light pollution. A faint companion is in orbit around the red giant star,[7] although it is not visible to the naked eye. Located near Alpha is Lambda Serpentis, a magnitude 4.42 star rather similar to the Sun[8] located only 12.12 parsecs (39.5 ly) away.[9] Another solar analog in Serpens is the primary of Psi Serpentis, a binary star[10] located slightly further away at approximately 14.64 parsecs (47.7 ly).[11]

Beta, Gamma, and Iota Serpentis form a distinctive triangular shape marking the head of the snake, with Kappa Serpentis being roughly midway between Gamma and Iota. The brighest of the four with an apparent magnitude of 3.67, Beta Serpentis is a white main-sequence star roughly 155.0 parsecs (506 ly) distant.[12] It is likely that a nearby star of magnitude 9.95[13] is physically associated with Beta, although it is not certain.[14] The Mira variable R Serpentis, located between Beta and Gamma, is visible to the naked eye at its maximum brightness of 5.16, but, typical of Mira variables, it can fade to below magnitude 14.[15] Gamma Serpentis itself is an F-type subgiant located only 11.25 parsecs (36.7 ly) distant and thus is quite bright, being of magnitude 3.84.[16] The star is known to show solar-like oscillations[17]

Delta Serpentis, forming part of the body of the snake between the heart and the head, is a multiple star system[18] located 69.93 parsecs (228.1 ly) from Earth. Consisting of four stars, the system has a total apparent magnitude of 3.79 as viewed from Earth,[19] although two of the stars, with a combined apparent magntitude of 3.80, provide nearly all the light that reaches Earth.[20] The primary, a white subgiant, is a Delta Scuti variable with an average apparent magnitude of 4.23.[21] Located very near Delta, both in the night sky and likely in actual space at an estimated distance of 70.87 parsecs (231.1 ly),[22] is the barium star 16 Serpentis.[23] Another notable variable star visible to the naked eye is Chi Serpentis, an Alpha2 Canum Venaticorum variable located midway between Delta and Beta which varies from its median brightness of 5.33 by 0.03 magnitudes over a period of approximately 1.5 days.[24]

The two stars in Serpens Caput that form part of the Snake's body below the heart are Epsilon and Mu Serpentis, both third-magnitude A-type main-sequence stars.[25][26] Both have a peculiarity: Epsilon is an Am star,[27] while Mu is a binary.[28] Located slightly northwest of Mu is 36 Serpentis, another A-type main-sequence star. This star also has a peculiarity; it is a binary with the primary component being a Lambda Boötis star, meaning that it has solar-like amounts of carbon, nitrogen, and oxygen, while containing very low amounts of iron peak elements.[29] 25 Serpentis, located a few degrees northeast of Mu Serpentis, is a spectroscopic binary[30] consisting of a hot B-type giant and an A-type main-sequence star. The primary is a slowly pulsating B star, which causes the system to vary by 0.03 magnitudes.[31]

Serpens Caput contains many RR Lyrae variables, although most are too faint to be seen without professional equipment. The brightest is VY Serpentis, only of 10th magnitude. Interestingly, this star's period has been increasing by approximately 1.2 seconds per century.[32] A variable star of a different kind is Tau4 Serpentis, a cool red giant that pulsates between magnitudes 5.89 and 7.07 in 87 days.[33] This star has been found to display an inverse P Cygni profile.[34]

Several stars in Serpens have been found to have planets. The brightest, Omega Serpentis, located between Epsilon and Mu, is an orange giant with a planet of approximately 1.7 Jupiter-masses.[35] NN Serpentis, an eclipsing post-common-envelope binary consisting of a white dwarf and a red dwarf,[36] is very likely to have two planets causing variations in the period of the eclipses.[37] Although it does not have a planet, the solar analog HD 137510 has been found to have a brown dwarf companion within the brown dwarf desert.[38]

PSR B1534+11 is a system consisting of two neutron stars orbiting each other, one of which is a pulsar with a period of 37.9 milliseconds. Located approximately 1,051 parsecs (3,430 ly) distant, the system demonstrates one of the best examples of general relativity.[39] The X-ray emission from the system has been found to be present when the non-pulsar star intersects the equatorial pulsar wind of the pulsar, and the system's orbit has been found to vary slightly.[40]

Tail stars[edit]

The constellation Serpens (Cauda) as it can be seen by the naked eye

The brightest star in the tail, Eta Serpentis, is similar to Alpha Serpentis' primary in that it is a red giant of spectral class K. This star, however, is known to exhibit solar-like oscillations over a period of approximately 2.16 hours.[41] Eta Serpentis was previously classified as a carbon star, which would have made it the brightest carbon star in the sky, although this classification was found to be erroneous.[42]

The other two stars in Serpens Cauda forming its asterism are Theta and Xi Serpentis. Xi, where the asterism crosses over to Mu Serpentis in the head, is a triple star system[7] located approximately 105.2 parsecs (343 ly) away.[43] Two of the stars, with a combined apparent magnitude of 3.54, form a spectroscopic binary, and thus cannot be resolved with modern equipment. The primary is a white giant with an excess of strontium.[43] Theta, forming the tip of the tail, is also a multiple system, consisting of two A-type main-sequence stars with a combined apparent magnitude of 4.10 separated by almost half an arcminute.[7]

Lying near the boundary with Ophiuchus are Zeta (23.55 parsecs (76.8 ly) distant), Nu (209.3 parsecs (683 ly) distant), and Omicron Serpentis (173.1 parsecs (565 ly) distant). All three are 4th-magnitude main-sequence stars, with Nu and Omicron being of spectral type A[44][45] and Zeta being of spectral type F.[46] Nu is a binary star[7] with a secondary component of magnitude 9.3,[47] while Omicron is a Delta Scuti variable with amplitude variations of 0.01 magnitudes.[48] In 1909, the symbiotic nova[49] RT Serpentis appeared near Omicron, although it only reached a maximum magnitude of 10.2.[50]

The star system 59 Serpentis, also known as d Serpentis, is a triple star system [51] consisting of a spectroscopic binary containing an A-type star and an orange giant[52] and an orange giant secondary.[53] The system shows irregular variations in brightness between magnitudes 5.17 and 5.2.[54] In 1970, the nova FH Serpentis appeared just slightly north of 59 Serpentis, reaching a maximum brightness of 4.5.[55] Also near 59 Serpentis in the Serpens Cloud are several Orion variables. MWC 297 is a Herbig Be star that in 1994 exhibited a large X-ray flare and increased in X-ray luminosity by five times before returning to the quiescent state.[56] The star also appears to possess a circumstellar disk.[57] Another Orion variable in the region is VV Serpentis, a Herbig Ae star that has been found to exhibit Delta Scuti pulsations.[58] VV Serpentis has also, like MWC 297, been found to have a dusty disk surrounding it,[59] and is also a UX Orionis star,[60] meaning that it shows irregular variations in its brightness.

The star HR 6958, also known as MV Serpentis, is an Alpha2 Canum Venaticorum variable that is faintly visible to the naked eye.[61] The star's metal abundance is incredibly high for most metals at the iron peak and heavier, and has also been found to contain excess silicon.[62] Barely visible to the naked eye is HD 172365,[63] a likely post-blue straggler in the open cluster IC 4756 that contains a large excess of lithium.[64] HD 172189, also located in IC 4756, is an Algol variable eclipsing binary[65] with a 5.70 day period. The primary star in the system is also a Delta Scuti variable, undergoing multiple pulsation frequencies, which, combined with the eclipses, causes the system to vary by around a tenth of a magnitude.[66]

As the Milky Way passes through it, Serpens Cauda contains many massive OB stars. Several of these are visible to the naked eye, such as NW Serpentis, an early Be star that has been found to be somewhat variable. The variability is interesting; according to one study, it could be one of the first discovered hybrids between Beta Cephei variables and slowly pulsating B stars.[67] Although not visible to the naked eye, HD 167971 (MY Serpentis) is a Beta Lyrae variable triple system consisting of three very hot O-type stars. A member of the cluster NGC 6604,[68] the two eclipsing stars are both blue giants, with one being of the very early spectral type O7.5III. The remaining star is either a blue giant or supergiant of a late O or early B spectral type.[65] Also an eclipsing[69] binary, the HD 166734 system consists of two O-type blue supergiants in orbit around each other.[70] Less extreme in terms of mass and temperature is HD 161701, a spectroscopic binary consisting of a B-type primary and an Ap secondary, although it is the only known spectroscopic binary to consist of a star with excess of mercury and manganese and an Ap star.[71]

South of the Eagle Nebula on the border with Sagittarius is the eclipsing binary W Serpentis, whose primary is a white giant that is interacting with the secondary. The system has been found to contain an accretion disk, and was one of the first discovered Serpentids, which are eclipsing binaries containing exceptionally strong far-ultraviolet spectral lines.[72] It is suspected that such Serpentids are in an earlier evolutionary phase, and will evolve first into double periodic variables and then classical Algol variables.[73] Also near the Eagle Nebula is the eclipsing Wolf–Rayet binary CV Serpentis, consisting of a Wolf–Rayet star and a hot O-type subgiant. The system is surrounded by a ring-shaped nebula, likely formed during the Wolf–Rayet phase of the primary.[74] The eclipses of the system very erratic, and although there are two theories as to why, neither of them is completely consistent with current understanding of stars.[75]

Serpens Cauda contains a few X-ray binaries. One of these, GX 17+2, is a low-mass X-ray binary consisting of a neutron star and, as in all low-mass X-ray binaries, a low-mass star. The system has been classified as a Sco-like Z source, meaning that its accretion is near the Eddington limit.[76] The system has also been found to approximately every 3 days brighten by around 3.5 K-band magnitudes, possibly due to the presence of a synchrotron jet.[77] Another low-mass X-ray binary, Serpens X-1, undergoes occasional X-ray bursts. One in particular lasted nearly four hours, possibly explained by the burning of carbon in "a heavy element ocean".[78]

Deep-sky objects[edit]

Head objects[edit]

Messier 5, a naked-eye globular cluster in Serpens Caput

As the Milky Way does not pass through this part of Serpens, a view to many galaxies beyond it is possible. However, a few structures of the Milky Way Galaxy are present in Serpens Caput, such as Messier 5, a globular cluster located approximately 8° southwest of α Serpentis, next to the star 5 Serpentis. Barely visible to the naked eye under good conditions,[79] and is located approximately 25000 ly distant.[80] Messier 5 contains a large number of known RR Lyrae variable stars,[81] and is receding from us at over 50 km/s.[82] Interestingly, the cluster contains two millisecond pulsars, one of which is in a binary.[83] The cluster has been used to test for magnetic dipole moments in neutrinos, which could shed light on some hypothetical particles such as the axion.[84] Another globular cluster is Palomar 5, located just south of Messier 5. Interestingly, many stars are leaving this globular cluster due to the Milky Way's gravity, forming a tidal tail over 30,000 light-years (9,200 pc) long.[85]

A remarkable dark nebula complex is the L134/L183 complex. Along with a third cloud, they are likely fragments of a single original cloud located 36 degrees away from the galactic plane, a large distance for dark nebulae.[86] The entire complex is thought to be around 141 parsecs (460 ly) distant.[87] L183, also referred to as L134N, is particularly interesting; there are several infrared sources within, indicating pre-stellar sources[88] thought to present the first known observation of the contraction phase between cloud cores and prestellar cores.[89] The core is split into three regions,[90] with a combined mass of around 25 solar masses.[91]

Outside of the Milky Way, there are no bright deep-sky objects for amateur astronomers in Serpens Caput, with nothing else above 10th magnitude. The brightest is NGC 5962, a spiral galaxy located around 28 megaparsecs distant[92] with an apparent magnitude of 11.34.[93] Slightly fainter is NGC 5921, a barred spiral galaxy with a LINER-type active galactic nucleus located somewhat closer at a distance of 21 megaparsecs.[94] A type II supernova was observed in this galaxy in 2001 and was designated SN 2001X.[95] Fainter still are the spirals NGC 5964[96] and NGC 6118, with the latter being host to the supernova SN 2004dk.[97]

Hoag's Object, a galaxy in Serpens and a member of the very rare class known as ring galaxies

Hoag's Object, located 600 million light-years from Earth, is one of the most famous of a very rare class of galaxies known as ring galaxies. The outer ring is largely composed of young blue stars while the core is made up of older yellow stars. The predominant theory regarding its formation is that the progenitor galaxy was a barred spiral galaxy whose arms had velocities too great to keep the galaxy's coherence and therefore detached.[98] Arp 220 is another unusual galaxy in Serpens. The prototypical ultraluminous infrared galaxy, Arp 220 is located 250 million light-years from Earth. It consists of two large spiral galaxies in the process of colliding with their nuclei orbiting at a distance of 1,200 light-years, causing extensive star formation throughout both components. It possesses a large cluster of more than a billion stars, partially covered by thick dust clouds near one of the galaxies' core.[98] Another interacting galaxy pair, albeit in an earlier stage, consists of the galaxies NGC 5953 and NGC 5954. In this case, both are active galaxies, with the former a Seyfert 2 galaxy and the latter a LINER-type galaxy. Both are undergoing a burst of star formation triggered by the interaction.[99]

Seyfert's Sextet is a group of six galaxies, four of which are interacting gravitationally and two of which simply appear to be a part of the group despite their greater distance. The gravitationally bound cluster lies at a distance of 190 million light-years from Earth and is approximately 100,000 light-years across, making Seyfert's Sextet one of the densest galaxy group known. Astronomers predict that the four interacting galaxies will eventually merge to form a large elliptical galaxy.[98] The radio source 3C 326 was originally though to emanate from a giant elliptical galaxy. However, in 1990, it was shown that the source is instead a brighter, smaller galaxy a few arcseconds north.[100] This object, designated 3C 326 N, has enough gas for star formation, but is being inhibited due to the energy from the radio galaxy nucleus.[101]

A much larger galaxy cluster is Abell 2063. With a redshift of 0.0354,[102] it is located approximately 150,000,000 parsecs (490,000,000 ly) away from Earth. The cluster is thought to be interacting with the nearby galaxy group MKW 3s, based on radial velocity measurements of galaxies and the location of the cD galaxy at the center of Abell 2063.[103] The active galaxy at the center of MKW 3s — NGC 5920 — appears to be creating a bubble of hot gas from its radio activity.[104] Near the 5th-magnitude star Pi Serpentis lies AWM 4, a cluster containing an excess of metals in the intracluster medium. The central galaxy, NGC 6051, is a radio galaxy that is probably responsible for this enrichment.[105] Similar to AWM 4, the cluster Abell 2052 has central cD radio galaxy, 3C 317. Interestingly, this radio galaxy is believed to have restarted after a period of inactivity less than 200 years ago.[106] The galaxy has over 40,000 known globular clusters, the highest known total of any galaxy as of 2002.[107]

A composite image of 3C 321, a merging active galaxy pair

Consisting of two quasars with a separation of less than 5 arcseconds, the quasar pair 4C 11.50 is one of the visually closest pairs of quasars in the sky. The two have markedly different redshifts, however, and are thus unrelated.[108] The foreground member of the pair (4C 11.50 A) does not have enough mass to refract light from the background component (4C 11.50 B) enough to produce a lensed image, although it does have a true companion of its own.[109] An even stranger galaxy pair is 3C 321. Unlike the previous pair, the two galaxies making up 3C 321 are interacting with each other and are in the process of merging. Interestingly, both members appear to be active galaxies; the primary radio galaxy may be responsible for the activity in the secondary by means of the former's jet driving material onto the latter's supermassive black hole.[110]

A remarkable example of gravitational lensing is found in the radio galaxy 3C 324. First thought to be a single overluminous radio galaxy with a redshift of z = 1.206, it was found in 1987 to actually be two galaxies, with the radio galaxy at the aforementioned redshift being lensed by another galaxy at redshift z = 0.845. The first example of a multiply-imaged radio galaxy discovered,[111] the source appears to be an elliptical galaxy with a dust lane obscuring our view of the visual and ultraviolet emission from the nucleus.[112] In even shorter wavelengths, the BL Lac object PG 1553+113 is a heavy emitter of gamma rays. This object is the most distant found to emit photons with energies in the TeV range as of 2007.[113] The spectrum is unique, with hard emission in some ranges of the gamma-ray spectrum in stark contrast to soft emission in others.[114] In 2012, the object flared in the gamma-ray spectrum, tripling in luminosity for two nights, allowing the redshift to be accurately measured as z = 0.49.[115]

Several gamma-ray bursts (GRBs) have been observed in Serpens Caput, such as GRB 970111, one of the brightest GRBs observed. Interestingly, an optical transient event associated with this GRB has not been found, despite its intensity. The host galaxy initially also proved elusive, however it now appears that the host is a Seyfert I galaxy located at redshift z = 0.657.[116] The X-ray afterglow of the GRB has also been much fainter than for other dimmer GRBs.[117] More distant is GRB 060526 (redshift z = 3.221), from which X-ray and optical afterglows were detected. This GRB was surprisingly faint for a long-duration GRB.[118]

Tail objects[edit]

The Pillars of Creation, a well-known star-forming region in the Eagle Nebula made famous by this Hubble photograph

Part of the Milky Way passes through the tail, and thus Serpens Cauda is rich in deep-sky objects within our own galaxy. The Eagle Nebula and its associated star cluster, Messier 16 lie 7,000 light-years from Earth in the direction of the galactic center. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. The stars being born in the Eagle Nebula, added to those with an approximate age of 5 million years have an average temperature of 45,000 kelvins and produce prodigious amounts of radiation that will eventually destroy the dust pillars.[98] Despite its fame, the Eagle Nebula is fairly dim, with an integrated magnitude of approximately 6.0. The star-forming regions in the nebula are often evaporating gaseous globules; unlike Bok globules they only hold one protostar.[119]

North of Messier 16, at a distance of approximately 1,900 parsecs (6,200 ly), is the OB association Serpens OB2, containing over 100 OB stars. Around 5 million years old, the association appears to still contain star-forming regions, and the light from its stars is illuminating the HII region S 54.[120] Within this HII region is the open cluster NGC 6604, which is the same age as the surrounding OB association,[121] and the cluster is now thought to simply be the densest part of it.[122] Interestingly, the cluster appears to be producing a thermal chimney of ionized gas, caused by the interaction of the gas from the galactic disk with the galactic halo.[120]

Another open cluster in Serpens Cauda is IC 4756, containing at least one naked-eye star (HD 172365)[123] (another naked-eye star in the vicinity, HD 171586, is most likely likely unrelated). Located approximately 437 parsecs (1,430 ly) distant,[124] the cluster is estimated to be around 800 million years old, which is quite old for an open cluster.[125] Despite the presence of the Milky Way in Serpens Cauda, one globular cluster can be found: NGC 6535, although invisible to the naked eye, can be made out in small telescopes just north of Zeta Serpentis. Rather small and sparse for a globular cluster,[126] this cluster contains no known RR Lyrae variables, which is unusual for a globular cluster.[127]

The Red Square Nebula, one of the very few near-perfect squares in astronomy

MWC 922 is a star surrounded by a planetary nebula. Dubbed the Red Square Nebula due to its similarities to the Red Rectangle Nebula, the planetary nebula appears to be a nearly perfect square with a dark band around the equatorial regions. The nebula contains concentric rings, which are similar to those seen in the supernova SN 1987A.[128] MWC 922 itself is an FS Canis Majoris variable,[129] meaning that it is a Be star containing exceptionally bright hydrogen emission lines as well as select forbidden lines, likely due to the presence of a close binary.[130] East of Xi Serpentis is another planetary nebula, Abell 41, containing the binary star MT Serpentis at its center. The nebula appears to have a bipolar structure, and the axis of symmetry of the nebula has been found to be within 5° of the line perpendicular to the orbital plane of the stars, strengthening the link between binary stars and bipolar planetary nebulae.[131] On the other end of the stellar age spectrum is L483, a dark nebula which contains the protostar IRAS 18418-0440. Although classified as a class 0 protostar, it has some unusual features for such an object, such as a lack of high-velocity stellar winds, and it has been proposed that this object is in transition between class 0 and class I.[132] A variable nebula exists around the protostar, although it is only visible in infrared light.[133]

Westerhout 40, one of the nearest sites of massive star formation

The Serpens cloud is a massive star-forming molecular cloud located in the southern part of Serpens Cauda. Only two million years old[134] and 415 parsecs (1,350 ly) distant,[135] the cloud is known to contain many protostars such as Serpens FIRS 1[136] and Serpens SVS 20.[137] The Serpens South protocluster was uncovered by NASA's Spitzer Space Telescope in the southern portion of the cloud,[138] and it appears that star formation is still continuing in the region.[139] Another location of star formation is the Westerhout 40 complex, consisting of a prominent HII region adjacent to a molecular cloud.[140] Located around 500 parsecs (1,600 ly) distant,[141] it is one of the nearest massive regions of star formation, but as the molecular cloud obscures the HII region, rendering it and its embedded cluster tough to see visibly, it is not as well-studied as others.[142] The embedded cluster likely contains over 600 stars above 0.1 solar masses,[143] with several massive stars, including at least one O-type star, being responsible for lighting the HII region and the production of a bubble.[141]

Despite the presence of the Milky Way, several active galaxies are visible in Serpens Cauda as well, such as PDS 456, located near Xi Serpentis. The most intrinsically luminous nearby active galaxy,[144] this AGN has been found to be extremely variable in the X-ray spectrum. This has allowed light to be shed on the nature of the supermassive black hole at the center, likely a Kerr black hole.[145] It is possible that the quasar is undergoing a transition from an ultraluminous infrared galaxy to a classical radio-quiet quasar, but there are problems with this theory, and the object appears to be an exceptional object that does not completely lie within current classification systems.[144] Nearby is NRAO 530, a blazar that has been known to flare in the X-rays occasionally. One of these flares was for less than 2000 seconds, making it the shortest flare ever observed in a blazar as of 2004.[146] The blazar also appears to show periodic variability in its radio wave output over two different periods of six and ten years.[147]

Meteor showers[edit]

There are two daytime meteor showers that radiate from Serpens, the Omega Serpentids and the Sigma Serpentids. Both showers peak between December 18 and December 25.[148]


  1. ^ a b c Ridpath, Ian. "Serpens". Star Tales. self-published. Retrieved 15 May 2014. 
  2. ^ Gavin White, Babylonian Star-Lore (2007), p. 180.
  3. ^ a b Ridpath, Ian. "Constellations: Andromeda–Indus". Star Tales. self-published. Retrieved 1 April 2014. 
  4. ^ "Caelum, Constellation Boundary". The Constellations (International Astronomical Union). Retrieved 20 April 2014. 
  5. ^ Russell, H. N. (1922). "The New International Symbols for the Constellations". Popular Astronomy 30: 469–71. Bibcode:1922PA.....30..469R. 
  6. ^ "* Alpha Serpentis – Star in double system". SIMBAD. Retrieved 18 April 2014. 
  7. ^ a b c d Eggleton, P. P.; Tokovinin, A. A. (2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869. doi:10.1111/j.1365-2966.2008.13596.x.  edit
  8. ^ Da Silva, R.; Porto De Mello, G. F.; Milone, A. C.; Da Silva, L.; Ribeiro, L. S.; Rocha-Pinto, H. J. (2012). "Accurate and homogeneous abundance patterns in solar-type stars of the solar neighbourhood: A chemo-chronological analysis". Astronomy & Astrophysics 542: A84. doi:10.1051/0004-6361/201118751.  edit
  9. ^ "* Lambda Serpentis – Star". SIMBAD. Retrieved 20 May 2014. 
  10. ^ Hall, J. C.; Henry, G. W.; Lockwood, G. W.; Skiff, B. A.; Saar, S. H. (2009). "The Activity and Variability of the Sun and Sun-Like Stars. Ii. Contemporaneous Photometry and Spectroscopy of Bright Solar Analogs". The Astronomical Journal 138: 312. doi:10.1088/0004-6256/138/1/312.  edit
  11. ^ "* Psi Serpentis – Double or multiple star". SIMBAD. Retrieved 21 June 2014. 
  12. ^ "* Beta Serpentis – Star in double system". SIMBAD. Retrieved 12 May 2014. 
  13. ^ "* Beta Serpentis B – Star in double system". SIMBAD. Retrieved 12 May 2014. 
  14. ^ Shaya, E. J.; Olling, R. P. (2011). "Very Wide Binaries and Other Comoving Stellar Companions: A Bayesian Analysis of Thehipparcoscatalogue". The Astrophysical Journal Supplement Series 192: 2. doi:10.1088/0067-0049/192/1/2.  edit
  15. ^ VSX (4 January 2010). "R Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 22 May 2014. 
  16. ^ "* Gamma Serpentis – Variable star". SIMBAD. Retrieved 22 May 2014. 
  17. ^ Bi, S. ‐L.; Basu, S.; Li, L. ‐H. (2008). "Seismological Analysis of the Stars γ Serpentis and ι Leonis: Stellar Parameters and Evolution". The Astrophysical Journal 673 (2): 1093. doi:10.1086/521575.  edit
  18. ^ Malkov, O. Y.; Tamazian, V. S.; Docobo, J. A.; Chulkov, D. A. (2012). "Dynamical masses of a selected sample of orbital binaries". Astronomy & Astrophysics 546: A69. doi:10.1051/0004-6361/201219774.  edit
  19. ^ "* Delta Serpentis – Double or multiple star". SIMBAD. Retrieved 18 May 2014. 
  20. ^ "* Delta Serpentis B – Star in double system". SIMBAD. Retrieved 18 May 2014. 
  21. ^ VSX (4 January 2010). "Delta Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 18 May 2014. 
  22. ^ "* 16 Serpentis – Star". SIMBAD. Retrieved 24 May 2014. 
  23. ^ Tomkin, J.; Lambert, D. L. (1986). "Heavy-element abundances in the mild barium stars Omicron Virginis and 16 Serpentis". The Astrophysical Journal 311: 819. doi:10.1086/164821.  edit
  24. ^ VSX (4 January 2010). "Chi Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 26 May 2014. 
  25. ^ "* Epsilon Serpentis – Star". SIMBAD. Retrieved 26 May 2014. 
  26. ^ "* Mu Serpentis – Star". SIMBAD. Retrieved 26 May 2014. 
  27. ^ Adelman, S. J.; Albayrak, B. (1998). "Elemental abundance analyses with DAO spectrograms -- XX. The early a stars   Serpentis, 29 Vulpeculae and   Aquarii". Monthly Notices of the Royal Astronomical Society 300 (2): 359. doi:10.1046/j.1365-8711.1998.01859.x.  edit
  28. ^ Gontcharov, G. A.; Kiyaeva, O. V. (2010). "Photocentric orbits from a direct combination of ground-based astrometry with Hipparcos II. Preliminary orbits for six astrometric binaries". New Astronomy 15 (3): 324. doi:10.1016/j.newast.2009.09.006.  edit
  29. ^ Nikolov, G.; Atanasova, E.; Iliev, I. K.; Paunzen, E.; Barzova, I. S. (April 2008). "Spectroscopic orbit determination of two metal-weak dwarf stars: HD64491 and HD141851". Contributions of the Astronomical Observatory Skalnaté Pleso 38 (2): 433–434. Bibcode:2008CoSka..38..433N. 
  30. ^ Petrie, R. M.; Phibbs, E. (1950). "Redetermination of the spectrographic orbits of iot Peg and 25 Ser.". Publications of the Dominion Astrophysical Observatory Victoria 8: 225. Bibcode:1950PDAO....8..225P. 
  31. ^ VSX; Otero, S. A (10 February 2012). "PT Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 28 May 2014. 
  32. ^ Wunder, E. (October 1991). "Period Changes of Bright RR Lyrae Stars SU Dra and VY Ser". Information Bulletin on Variable Stars 3669 (1): IBVS Homepage. Bibcode:1991IBVS.3669....1W. 
  33. ^ VSX; Otero, S. A (28 June 2012). "Tau4 Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 24 June 2014. 
  34. ^ Kolotilov, E. A.; Russev, R. M. (January 1980). "Inverse P Cyg Profile of Halpha in the Spectrum of the Red Giant HD 139216 = tau4 Ser". Information Bulletin on Variable Stars 1730: 1. Bibcode:1980IBVS.1730....1K. 
  35. ^ Sato, B.; Omiya, M.; Harakawa, H.; Liu, Y. -J.; Izumiura, H.; Kambe, E.; Takeda, Y.; Yoshida, M.; Itoh, Y.; Ando, H.; Kokubo, E.; Ida, S. (2013). "Planetary Companions to Three Evolved Intermediate-Mass Stars: HD 2952, HD 120084, and   Serpentis". Publications of the Astronomical Society of Japan 65 (4): 85. doi:10.1093/pasj/65.4.85.  edit
  36. ^ Parsons, S. G.; Marsh, T. R.; Copperwheat, C. M.; Dhillon, V. S.; Littlefair, S. P.; Gänsicke, B. T.; Hickman, R. (2010). "Precise mass and radius values for the white dwarf and low mass M dwarf in the pre-cataclysmic binary NN Serpentis". Monthly Notices of the Royal Astronomical Society 402 (4): 2591. doi:10.1111/j.1365-2966.2009.16072.x.  edit
  37. ^ Marsh, T. R.; Parsons, S. G.; Bours, M. C. P.; Littlefair, S. P.; Copperwheat, C. M.; Dhillon, V. S.; Breedt, E.; Caceres, C.; Schreiber, M. R. (2013). "The planets around NN Serpentis: Still there". Monthly Notices of the Royal Astronomical Society 437: 475. doi:10.1093/mnras/stt1903.  edit
  38. ^ Endl, Michael; Hatzes, Artie P.; Cochran, William D.; McArthur, Barbara; Prieto, Carlos Allende; Paulson, Diane B.; Guenther, Eike; Bedalov, Ana (2004). "HD 137510: An Oasis in the Brown Dwarf Desert". The Astrophysical Journal 611 (2): 1121. Bibcode:2004ApJ...611.1121E. doi:10.1086/422310. 
  39. ^ Fonseca, E.; Stairs, I. H.; Thorsett, S. E. (2014). "A Comprehensive Study of Relativistic Gravity Using Psr B1534+12". The Astrophysical Journal 787: 82. doi:10.1088/0004-637X/787/1/82.  edit
  40. ^ Durant, M.; Kargaltsev, O.; Volkov, I.; Pavlov, G. G. (2011). "Orbital Variation of the X-Ray Emission from the Double Neutron Star Binary J1537+1155". The Astrophysical Journal 741: 65. doi:10.1088/0004-637X/741/1/65.  edit
  41. ^ Hekker, S.; Aerts, C. (2010). "Line-profile variations of stochastically excited oscillations in four evolved stars". Astronomy and Astrophysics 515: A43. doi:10.1051/0004-6361/200912777.  edit
  42. ^ Antipova, L. I.; Boyarchuk, A. A. (2001). "The chemical composition of the red giant η Ser". Astronomy Reports 45 (9): 700. doi:10.1134/1.1398919.  edit
  43. ^ a b "Xi Serpentis – Spectroscopic binary". SIMBAD. Retrieved 21 June 2014. 
  44. ^ "Nu Serpentis – Star in double system". SIMBAD. Retrieved 20 June 2014. 
  45. ^ "Omicron Serpentis – Variable Star of delta Sct type". SIMBAD. Retrieved 20 June 2014. 
  46. ^ "Zeta Serpentis – Star". SIMBAD. Retrieved 20 June 2014. 
  47. ^ "BD-12 4724 – Star in double system". SIMBAD. Retrieved 20 June 2014. 
  48. ^ VSX (4 January 2010). "Omicron Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 20 June 2014. 
  49. ^ Pavlenko, E. P.; Bochkov, V. V.; Vasil'Yanovskaya, O. P. (1996). "9,6-Year periodicity of symbiotic nova RT Ser (1909) during the outburst decay from 1940 to 1994". Astrophysics 39: 15. doi:10.1007/BF02044949.  edit
  50. ^ VSX; Osborne, W. (1 April 2014). "RT Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 28 May 2014. 
  51. ^ Tilley, E. C. (1943). "A Spectrographic Study of the Triple System in 59 D Serpentis". The Astrophysical Journal 98: 347. doi:10.1086/144577.  edit
  52. ^ Abt, H. A. (2009). "Mk Classifications of Spectroscopic Binaries". The Astrophysical Journal Supplement Series 180: 117. doi:10.1088/0067-0049/180/1/117.  edit
  53. ^ "HD 169986 – Star in double system". SIMBAD. Retrieved 25 May 2014. 
  54. ^ VSX (4 January 2010). "d Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 25 May 2014. 
  55. ^ VSX (28 April 2010). "FH Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 23 June 2014. 
  56. ^ Hamaguchi, K.; Terada, H.; Bamba, A.; Koyama, K. (2000). "Large X‐Ray Flare from the Herbig Be Star MWC 297". The Astrophysical Journal 532 (2): 1111. doi:10.1086/308607.  edit
  57. ^ Acke, B.; Verhoelst, T.; Van Den Ancker, M. E.; Deroo, P.; Waelkens, C.; Chesneau, O.; Tatulli, E.; Benisty, M.; Puga, E.; Waters, L. B. F. M.; Verhoeff, A.; De Koter, A. (2008). "MWC 297: A young high-mass star rotating at critical velocity". Astronomy and Astrophysics 485: 209. doi:10.1051/0004-6361:200809654.  edit
  58. ^ Ripepi, V.; Bernabei, S.; Marconi, M.; Ruoppo, A.; Palla, F.; Monteiro, M. J. P. F. G.; Marques, J. P.; Ferrara, P.; Marinoni, S.; Terranegra, L. (2007). "Discovery of δ Scuti pulsation in the Herbig Ae star VV Serpentis". Astronomy and Astrophysics 462 (3): 1023. doi:10.1051/0004-6361:20065728.  edit
  59. ^ Alonso‐Albi, T.; Fuente, A.; Bachiller, R.; Neri, R.; Planesas, P.; Testi, L. (2008). "The Dusty Disk around VV Serpens". The Astrophysical Journal 680 (2): 1289. doi:10.1086/587935.  edit
  60. ^ VSX; Otero, S. A. (23 November 2011). "VV Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 28 May 2014. 
  61. ^ VSX (4 January 2010). "MV Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 25 May 2014. 
  62. ^ López-García, Z.; Adelman, S. J.; Pintado, O. I. (2001). "Elemental abundance studies of CP stars". Astronomy and Astrophysics 367 (3): 859–864. Bibcode:2001A&A...367..859L. doi:10.1051/0004-6361:20000438.  edit
  63. ^ "HR 7008 – Star in Cluster". SIMBAD. Retrieved 14 December 2014. 
  64. ^ Andrievsky, S. M.; Gorlova, N. I.; Klochkova, V. G.; Kovtyuch, V. V.; Panchuk, V. E. (1999). "The Lithium-rich supergiant HD172365". Astronomische Nachrichten 320 (1): 35. Bibcode:1999AN....320...35A. doi:10.1002/1521-3994(199903)320:1<35::aid-asna35>;2-f. 
  65. ^ a b IbanoǧLu, C.; Evren, S.; Taş, G.; Çakırlı, Ö.; Bozkurt, Z.; Afşar, M.; Sipahi, E.; Dal, H. A.; Özdarcan, O.; Çamurdan, D. Z.; Çamurdan, M.; Frasca, A. (2009). "Spectroscopic and photometric observations of the selected Algol-type binaries★- IV. V799 Cassiopeiae, BX Piscium and HD 172189". Monthly Notices of the Royal Astronomical Society 392 (2): 757. doi:10.1111/j.1365-2966.2008.14087.x.  edit
  66. ^ Costa, J. E. S.; Michel, E.; Peña, J.; Creevey, O.; Li, Z. P.; Chevreton, M.; Belmonte, J. A.; Alvarez, M.; Fox Machado, L.; Parrao, L.; Pérez Hernéndez, F.; Fernández, A.; Fremy, J. R.; Pau, S.; Alonso, R. (2007). "Pulsational frequencies of the eclipsing δ Scuti star HD 172189. Results of the STEPHI XIII campaign". Astronomy and Astrophysics 468 (2): 637. doi:10.1051/0004-6361:20065784.  edit
  67. ^ Gutiérrez-Soto, J.; Fabregat, J.; Suso, J.; Suárez, J. C.; Moya, A.; Garrido, R.; Hubert, A. -M.; Floquet, M.; Neiner, C.; Frémat, Y. (2007). "Multiperiodic pulsations in the Be stars NW Serpentis and V1446 Aquilae". Astronomy and Astrophysics 472 (2): 565. doi:10.1051/0004-6361:20077414.  edit
  68. ^ De Becker, M.; Rauw, G.; Blomme, R.; Pittard, J. M.; Stevens, I. R.; Runacres, M. C. (2005). "An XMM-Newton observation of the multiple system HD 167971 (O5-8V + O5-8V + (O8I)) and the young open cluster NGC 6604". Astronomy and Astrophysics 437 (3): 1029. doi:10.1051/0004-6361:20052810.  edit
  69. ^ VSX (4 January 2010). "V411 Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 25 May 2014. 
  70. ^ Conti, P. S.; Ebbets, D.; Massey, P.; Niemela, V. S. (1980). "Spectroscopic studies of O-type binaries. V - the of System HD 166734". The Astrophysical Journal 238: 184. doi:10.1086/157971.  edit
  71. ^ Hubrig, S.; Carroll, T. A.; Gonzalez, J. F.; Scholler, M.; Ilyin, I.; Saffe, C.; Castelli, F.; Leone, F.; Giarrusso, M. (2014). "The magnetic field in HD 161701, the only binary system identified to consist of an Hg Mn primary and an Ap secondary". Monthly Notices of the Royal Astronomical Society: Letters 440: L6. Bibcode:2014MNRAS.440L...6H. doi:10.1093/mnrasl/slu012. 
  72. ^ Weiland, J. L.; Shore, S. N.; Beaver, E. A.; Lyons, R. W.; Rosenblatt, E. I. (1995). "Goddard High-Resolution Spectrograph Observations of the Interacting Binary System W Serpentis". The Astrophysical Journal 447: 401. doi:10.1086/175883.  edit
  73. ^ Mennickent, R. E.; Kolaczkowski, Z. (2009). "Interacting Binary Star Environments and the W Ser - DPV - Algol Connection". arXiv:0904.1539 [astro-ph.SR]. 
  74. ^ Cappa, C. E. (2002). "VLA Radio Continuum and [ITAL]IRAS[/ITAL] Observations of the Ring Nebulae around WR 101 and WR 113". The Astronomical Journal 123 (6): 3348–3355. doi:10.1086/340725.  edit
  75. ^ David-Uraz, Alexandre (2012). "Using MOST to reveal the secrets of the mischievous Wolf-Rayet binary CV Ser". Monthly Notices of the Royal Astronomical Society 426 (3): 1720–1730. doi:10.1111/j.1365-2966.2012.21736.x.  edit
  76. ^ Lin, Dacheng (2012). "THE SPECTRAL EVOLUTION ALONG THE Z TRACK OF THE BRIGHT NEUTRON STAR X-RAY BINARY GX 17+2". The Astrophysical Journal 756 (1): 34. doi:10.1088/0004-637X/756/1/34.  edit
  77. ^ Bornak, Jillian (2009). "A POSSIBLE PERIOD FOR THE K -BAND BRIGHTENING EPISODES OF GX 17+2". The Astrophysical Journal 701 (2): L110–L113. doi:10.1088/0004-637X/701/2/L110.  edit
  78. ^ Cornelisse, R. (2002). "A four-hours long burst from Serpens?X?1". Astronomy and Astrophysics 382 (1): 174–177. doi:10.1051/0004-6361:20011591.  edit
  79. ^ Frommert, H.; Kronberg, C. (21 August 2007). "Messier 5". SEDS. Retrieved 16 December 2014. 
  80. ^ Paust, N. E. Q.; Reid, I. N.; Piotto, G.; Aparicio, A.; Anderson, J.; Sarajedini, A.; Bedin, L. R.; Chaboyer, B.; Dotter, A.; Hempel, M.; Majewski, S.; Marín-Franch, A.; Milone, A.; Rosenberg, A.; Siegel, M. (2010). "The Acs Survey of Galactic Globular Clusters. Viii. Effects of Environment on Globular Cluster Global Mass Functions". The Astronomical Journal 139 (2): 476. doi:10.1088/0004-6256/139/2/476.  edit
  81. ^ Szeidl, B.; Hurta, Zs.; Jurcsik, J.; Clement, C.; Lovas, M. (2011). "Long-term photometric monitoring of Messier 5 variables - I. Period changes of RR Lyrae stars". Monthly Notices of the Royal Astronomical Society 411 (3): 1744. Bibcode:2011MNRAS.411.1744S. doi:10.1111/j.1365-2966.2010.17815.x. 
  82. ^ Harris, William E. (1996). "A Catalog of Parameters for Globular Clusters in the Milky Way". The Astronomical Journal 112: 1487. Bibcode:1996AJ....112.1487H. doi:10.1086/118116. 
  83. ^ Freire, P. C. C.; Wolszczan, A.; Van Den Berg, M.; Hessels, J. W. T. (2008). "A Massive Neutron Star in the Globular Cluster M5". The Astrophysical Journal 679 (2): 1433. doi:10.1086/587832.  edit
  84. ^ Viaux, N.; Catelan, M.; Stetson, P. B.; Raffelt, G. G.; Redondo, J.; Valcarce, A. A. R.; Weiss, A. (2013). "Particle-physics constraints from the globular cluster M5: Neutrino dipole moments". Astronomy & Astrophysics 558: A12. doi:10.1051/0004-6361/201322004.  edit
  85. ^ Ibata, R.; Gibson, B. (2007). "The Ghosts of Galaxies Past". Scientific American 296 (4): 40–5. doi:10.1038/scientificamerican0407-40. PMID 17479629.  edit
  86. ^ . doi:10.1086/159014.  Missing or empty |title= (help)
  87. ^ . Bibcode:1992BaltA...1..163C.  Missing or empty |title= (help)
  88. ^ . doi:10.1051/0004-6361:20021411.  Missing or empty |title= (help)
  89. ^ . doi:10.1051/0004-6361:20034087.  Missing or empty |title= (help)
  90. ^ . doi:10.1088/0004-637X/701/2/1044.  Missing or empty |title= (help)
  91. ^ . doi:10.1051/0004-6361:20011539.  Missing or empty |title= (help)
  92. ^ "NED results for object NGC 5962". NASA/IPAC Extragalactic Database. Retrieved 3 June 2015. 
  93. ^ Gil De Paz, Armando; Boissier, Samuel; Madore, Barry F.; Seibert, Mark; Joe, Young H.; Boselli, Alessandro; Wyder, Ted K.; Thilker, David; Bianchi, Luciana; Rey, Soo‐Chang; Rich, R. Michael; Barlow, Tom A.; Conrow, Tim; Forster, Karl; Friedman, Peter G.; Martin, D. Christopher; Morrissey, Patrick; Neff, Susan G.; Schiminovich, David; Small, Todd; Donas, Jose; Heckman, Timothy M.; Lee, Young‐Wook; Milliard, Bruno; Szalay, Alex S.; Yi, Sukyoung (2007). "TheGALEXUltraviolet Atlas of Nearby Galaxies". The Astrophysical Journal Supplement Series 173 (2): 185. Bibcode:2007ApJS..173..185G. doi:10.1086/516636. 
  94. ^ "NED results for object NGC 5921". NASA/IPAC Extragalactic Database. Retrieved 3 June 2015. 
  95. ^ Gal-Yam, A.; Shemmer, O.; Dann, J. (2001). "Supernova 2001X in NGC 5921". IAU Circ 7602: 2. Bibcode:2001IAUC.7602....2G. 
  96. ^ Hernández-Toledo, H. M.; Zendejas-Domínguez, J.; Avila-Reese, V. (2007). "BVRISurface Photometry of Isolated Spiral Galaxies". The Astronomical Journal 134 (6): 2286. Bibcode:2007AJ....134.2286H. doi:10.1086/521358. 
  97. ^ Stockdale, C. J.; Heim, M. S.; Vandrevala, C. M.; Bauer, F. E.; Van Dyk, S. D.; Weiler, K. W.; Pooley, D.; Immler, S.; Dwarkadas, V. (2009). "Supernovae 1996aq and 2004dk". Central Bureau Electronic Telegrams 1714: 1. Bibcode:2009CBET.1714....1S. 
  98. ^ a b c d Wilkins, Jamie; Dunn, Robert (2006). 300 Astronomical Objects: A Visual Reference to the Universe (1st ed.). Buffalo, New York: Firefly Books. ISBN 978-1-55407-175-3. 
  99. ^ Gonzalez Delgado, Rosa M.; Perez, Enrique (August 1996). "The circumnuclear region in the Seyfert 2 galaxy NGC 5953". Monthly Notices of the Royal Astronomical Society 281 (3): 781–798. Bibcode:1996MNRAS.281..781G. 
  100. ^ . Bibcode:1990MNRAS.246P..21R.  Missing or empty |title= (help)
  101. ^ . doi:10.1051/0004-6361/201423612.  Missing or empty |title= (help)
  102. ^ Kanov, Kalin N.; Sarazin, Craig L.; Hicks, Amalia K. (2006). "Chandra Observation of the Interaction of the Radio Source and Cooling Core in Abell 2063". The Astrophysical Journal 653: 184. Bibcode:2006ApJ...653..184K. doi:10.1086/508862. 
  103. ^ Krempec-Krygier, J.; Krygier, B. (1999). "Interaction of Abell Cluster 2063 and the Group of Galaxies MKW3s". Acta Astronomica 49: 403. Bibcode:1999AcA....49..403K. 
  104. ^ Giacintucci, S.; Mazzotta, P.; Brunetti, G.; Venturi, T.; Bardelli, S. (2006). "Evidence of gas heating by the central AGN in MKW 3s". Astronomische Nachrichten 327 (5–6): 573. Bibcode:2006AN....327..573G. doi:10.1002/asna.200610594. 
  105. ^ o’Sullivan, Ewan; Giacintucci, Simona; David, Laurence P.; Vrtilek, Jan M.; Raychaudhury, Somak (2011). "A deep Chandra observation of the poor cluster AWM 4 - II. The role of the radio jets in enriching the intracluster medium". Monthly Notices of the Royal Astronomical Society 411 (3): 1833. Bibcode:2011MNRAS.411.1833O. doi:10.1111/j.1365-2966.2010.17812.x. 
  106. ^ Venturi, T.; Dallacasa, D.; Stefanachi, F. (2004). "Radio galaxies in cooling core clusters. Renewed activity in the nucleus of 3C?317?". Astronomy and Astrophysics 422 (2): 515. Bibcode:2004A&A...422..515V. doi:10.1051/0004-6361:20040089. 
  107. ^ Lee, Myung Gyoon; Kim, Eunhyeuk; Geisler, Doug; Bridges, Terry; Ashman, Keith (2002). "A Comparative Study of Globular Cluster Systems in UGC 9799 and NGC 1129". Extragalactic Star Clusters 207: 330. Bibcode:2002IAUS..207..330L. 
  108. ^ Shaver, P. A.; Robertson, J. G. (1985). "The close QSO pair Q1548 + 114A, B". Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711) 212: 15P. Bibcode:1985MNRAS.212P..15S. 
  109. ^ Claeskens, J.-F.; Lee, D.-W.; Remy, M.; Sluse, D.; Surdej, J. (2000). "QSO mass constraints from gravitational lensing studies of quasar pairs. The cases of Q1548+114 A & B and Q1148+0055 A & B". Astronomy and Astrophysics 356: 840. Bibcode:2000A&A...356..840C. 
  110. ^ Evans, Daniel A.; Fong, Wen‐Fai; Hardcastle, Martin J.; Kraft, Ralph P.; Lee, Julia C.; Worrall, Diana M.; Birkinshaw, Mark; Croston, Judith H.; Muxlow, Tom W. B. (2008). "A Radio through X‐Ray Study of the Jet/Companion‐Galaxy Interaction in 3C 321". The Astrophysical Journal 675 (2): 1057. Bibcode:2008ApJ...675.1057E. doi:10.1086/527410. 
  111. ^ Fèvre, O. Le; Hammer, F.; Nottale, L.; Mathez, G. (March 25, 1987). "Is 3C324 the first gravitationally lensed giant galaxy?". Nature 326 (6110): 268–269. doi:10.1038/326268a0. 
  112. ^ Yamada, Toru; Kajisawa, Masaru; Tanaka, Ichi; Maihara, Toshinori; Iwamuro, Fumihide; Terada, Hiroshi; Goto, Miwa; Motohara, Kentaro; Tanabe, Hirohisa (02/01/2000). "High-Resolution Near-Infrared Imaging of the Powerful Radio Galaxy 3C 324 at z = 1.21 with the Subaru Telescope". Publications of the Astronomical Society of Japan (in English) 52 (1): 43–51. doi:10.1093/pasj/52.1.43. ISSN 0004-6264.  Check date values in: |date= (help)
  113. ^ . doi:10.1051/0004-6361:20078290.  Missing or empty |title= (help)
  114. ^ . doi:10.1088/0004-637X/708/2/1310.  Missing or empty |title= (help)
  115. ^ . doi:10.1088/0004-637X/802/1/65.  Missing or empty |title= (help)
  116. ^ Gorosabel, J.; Castro-Tirado, A. J.; Wolf, C.; Heidt, J.; Seitz, T.; Thommes, E.; Bartolini, C.; Guarnieri, A.; Masetti, N.; Piccioni, A.; Larsen, S.; Costa, E.; Feroci, M.; Frontera, F.; Palazzi, E.; Lund, N. (1998). "An optical study of the GRB 970111 field beginning 19 hours after the gamma-ray burst". Astronomy and Astrophysics 339: 719. Bibcode:1998A&A...339..719G. 
  117. ^ Feroci, M.; Antonelli, L. A.; Guainazzi, M.; Muller, J. M.; Costa, E.; Piro, L.; In 't Zand, J. J. M.; Frontera, F.; Dal Fiume, D.; Nicastro, L.; Orlandini, M.; Palazzi, E.; Zavattini, G.; Giommi, P.; Parmar, A. N.; Owens, A.; Castro-Tirado, A. J.; MacCarone, M. C.; Butler, R. C. (1998). "BeppoSAX follow-up search for the X-ray afterglow of GRB970111". Astronomy and Astrophysics 332: L29. Bibcode:1998A&A...332L..29F. 
  118. ^ Thöne, C. C.; Kann, D. A.; Jóhannesson, G.; Selj, J. H.; Jaunsen, A. O.; Fynbo, J. P. U.; Akerlof, C. W.; Baliyan, K. S.; Bartolini, C.; Bikmaev, I. F.; Bloom, J. S.; Burenin, R. A.; Cobb, B. E.; Covino, S.; Curran, P. A.; Dahle, H.; Ferrero, A.; Foley, S.; French, J.; Fruchter, A. S.; Ganesh, S.; Graham, J. F.; Greco, G.; Guarnieri, A.; Hanlon, L.; Hjorth, J.; Ibrahimov, M.; Israel, G. L.; Jakobsson, P. et al. (2010). "Photometry and spectroscopy of GRB 060526: A detailed study of the afterglow and host galaxy of az = 3.2 gamma-ray burst". Astronomy & Astrophysics 523: A70. Bibcode:2010A&A...523A..70T. doi:10.1051/0004-6361/200810340. 
  119. ^ Levy 2005, pp. 112-113.
  120. ^ a b Forbes, D. (2000). "The Serpens OB2 Association and Its Thermal "Chimney"". The Astronomical Journal 120 (5): 2594. doi:10.1086/316822.  edit
  121. ^ Barbon, R.; Carraro, G.; Munari, U.; Zwitter, T.; Tomasella, L. (2000). "Spectroscopy and BVIC photometry of the young open cluster NGC�6604". Astronomy and Astrophysics Supplement Series 144 (3): 451. doi:10.1051/aas:2000193.  edit
  122. ^ Reipurth, B. (2008). "The Young Cluster NGC 6604 and the Serpens OB2 Association". Handbook of Star Forming Regions, Volume II: the Southern Sky ASP Monograph Publications 5: 590. 
  123. ^ Herzog, A. D.; Sanders, W. L.; Seggewiss, W. (1975). "Membership and photometry of the open cluster IC 4756". Astronomy and Astrophysics 19: 211–234. Bibcode:1975A&AS...19..211H. 
  124. ^ Alcaino, G. (1965). "A photoelectric investigation of the galactic clusters IC 4665 and IC 4756". Bulletin / Lowell Observatory 6 (7): 167–172. Bibcode:1965LowOB...6..167A. 
  125. ^ Phelps, R. L.; Janes, K. A.; Montgomery, K. A. (1994). "Development of the Galactic disk: A search for the oldest open clusters". The Astronomical Journal 107: 1079. doi:10.1086/116920.  edit
  126. ^ Testa, Vincenzo; Corsi, Carlo E.; Andreuzzi, Gloria; Iannicola, Giacinto; Marconi, Gianni; Piersimoni, Anna Marina; Buonanno, Roberto (2001). "Horizontal-Branch Morphology and Dense Environments: [ITAL]HUBBLE SPACE TELESCOPE[/ITAL][ITAL]Hubble Space Telescope[/ITAL] Observations of Globular Clusters NGC 2298, 5897, 6535, and 6626". The Astronomical Journal 121 (2): 916. Bibcode:2001AJ....121..916T. doi:10.1086/318752. 
  127. ^ Sarajedini, Ata (1994). "CCD Photometry of the Galactic globular cluster NGC 6535 in the B and V Passbands". Publications of the Astronomical Society of the Pacific 106: 404. doi:10.1086/133392. 
  128. ^ Tuthill, P. G.; Lloyd, J. P. (2007). "A Symmetric Bipolar Nebula Around MWC 922". Science 316 (5822): 247. doi:10.1126/science.1135950. PMID 17431173.  edit
  129. ^ Plummer, A.; Otero, S. A. (27 March 2013). "MWC 922". AAVSO Website. American Association of Variable Star Observers. Retrieved 11 May 2014. 
  130. ^ Otero, S. A.; Watson, C.; Wils, P. "Variable Star Type Designations in the VSX". AAVSO Website. American Association of Variable Star Observers. Retrieved 11 May 2014. 
  131. ^ Jones, D.; Lloyd, M.; Santander-García, M.; López, J. A.; Meaburn, J.; Mitchell, D. L.; O'Brien, T. J.; Pollacco, D.; Rubio-Díez, M. M.; Vaytet, N. M. H. (2010). "Abell 41: Shaping of a planetary nebula by a binary central star★". Monthly Notices of the Royal Astronomical Society 408 (4): 2312. doi:10.1111/j.1365-2966.2010.17277.x.  edit
  132. ^ Tafalla, M.; Myers, P. C.; Mardones, D.; Bachiller, R. (2000). "L483: A protostar in transition from Class 0 to Class I". Astronomy and Astrophysics 359: 967. Bibcode:2000A&A...359..967T. 
  133. ^ Connelley, M. S.; Hodapp, K. W.; Fuller, G. A. (2009). "A Photometrically and Morphologically Variable Infrared Nebula in L483". The Astronomical Journal 137 (3): 3494. doi:10.1088/0004-6256/137/3/3494.  edit
  134. ^ Oliveira, I.; Merín, B.; Pontoppidan, K. M.; Van Dishoeck, E. F. (2013). "The Physical Structure of Protoplanetary Disks: The Serpens Cluster Compared with Other Regions". The Astrophysical Journal 762 (2): 128. doi:10.1088/0004-637X/762/2/128.  edit
  135. ^ Dzib, S.; Loinard, L.; Mioduszewski, A. J.; Boden, A. F.; Rodríguez, L. F.; Torres, R. M. (2010). "VLBA DETERMINATION OF THE DISTANCE TO NEARBY STAR-FORMING REGIONS. IV. A PRELIMINARY DISTANCE TO THE PROTO-HERBIG Ae Be STAR EC 95 IN THE SERPENS CORE". The Astrophysical Journal 718 (2): 610. doi:10.1088/0004-637X/718/2/610.  edit
  136. ^ Dionatos, O.; Jørgensen, J. K.; Teixeira, P. S.; Güdel, M.; Bergin, E. (2014). "Atomic jet from SMM1 (FIRS1) in Serpens uncovers protobinary companion". Astronomy & Astrophysics 563: A28. doi:10.1051/0004-6361/201322799.  edit
  137. ^ Ciardi, D. R.; Telesco, C. M.; Packham, C.; Gomez Martin, C.; Radomski, J. T.; De Buizer, J. M.; Phillips, C. J.; Harker, D. E. (2005). "Crystalline Silicate Emission in the Protostellar Binary Serpens SVS 20". The Astrophysical Journal 629 (2): 897. doi:10.1086/431548.  edit
  138. ^ Gutermuth, R. A.; Bourke, T. L.; Allen, L. E.; Myers, P. C.; Megeath, S. T.; Matthews, B. C.; Jørgensen, J. K.; Di Francesco, J.; Ward-Thompson, D.; Huard, T. L.; Brooke, T. Y.; Dunham, M. M.; Cieza, L. A.; Harvey, P. M.; Chapman, N. L. (2008). "The Spitzer Gould Belt Survey of Large Nearby Interstellar Clouds: Discovery of a Dense Embedded Cluster in the Serpens-Aquila Rift". The Astrophysical Journal 673 (2): L151. doi:10.1086/528710.  edit
  139. ^ Nakamura, F.; Sugitani, K.; Shimajiri, Y.; Tsukagoshi, T.; Higuchi, A.; Nishiyama, S.; Kawabe, R.; Takami, M.; Karr, J. L.; Gutermuth, R. A.; Wilson, G. (2011). "Molecular Outflows from the Protocluster Serpens South". The Astrophysical Journal 737 (2): 56. doi:10.1088/0004-637X/737/2/56.  edit
  140. ^ . doi:10.1086/156207.  Missing or empty |title= (help)
  141. ^ a b . doi:10.1088/0004-6256/144/4/116.  Missing or empty |title= (help)
  142. ^ .  Missing or empty |title= (help)
  143. ^ . doi:10.1088/0004-637X/725/2/2485.  Missing or empty |title= (help)
  144. ^ a b Yun, M. S.; Reddy, N. A.; Scoville, N. Z.; Frayer, D. T.; Robson, E. I.; Tilanus, R. P. J. (2004). "Multiwavelength Observations of the Gas‐rich Host Galaxy of PDS 456: A New Challenge for the ULIRG‐to‐QSO Transition Scenario". The Astrophysical Journal 601 (2): 723. doi:10.1086/380559.  edit
  145. ^ Reeves, J. N.; Wynn, G.; O'Brien, P. T.; Pounds, K. A. (2002). "Extreme X-ray variability in the luminous quasar PDS 456". Monthly Notices of the Royal Astronomical Society 336 (3): L56. doi:10.1046/j.1365-8711.2002.06038.x.  edit
  146. ^ Foschini, L.; Pian, E.; Maraschi, L.; Raiteri, C. M.; Tavecchio, F.; Ghisellini, G.; Tosti, G.; Malaguti, G.; Di Cocco, G. (2006). "A short hard X-ray flare from the blazar NRAO 530 observed by INTEGRAL". Astronomy and Astrophysics 450: 77. doi:10.1051/0004-6361:20064804.  edit
  147. ^ Lu, J. C.; Wang, J. Y.; An, T.; Lin, J. M.; Qiu, H. B. (2012). "Periodic radio variability in NRAO 530: Phase dispersion minimization analysis". Research in Astronomy and Astrophysics 12 (6): 643. doi:10.1088/1674-4527/12/6/004.  edit
  148. ^ Jenniskens, Peter (September 2012). "Mapping Meteoroid Orbits: New Meteor Showers Discovered". Sky & Telescope: 24. 

External links[edit]

Coordinates: Sky map 17h 00m 00s, +03° 00′ 00″