Hubbry Logo
Sagittarius B2Sagittarius B2Main
Open search
Sagittarius B2
Community hub
Sagittarius B2
logo
7 pages, 0 posts
0 subscribers
Be the first to start a discussion here.
Be the first to start a discussion here.
Sagittarius B2
Sagittarius B2
Sagittarius B2
View on Wikipedia
from Wikipedia
Sagittarius B2
Molecular cloud
Giant molecular cloud
Sagittarius B2
James Webb Space Telescope Mid-Infrared Instrument image of star-formation in Sagittarius B2. North is on the right side of this image.
Observation data: J2000.0[1] epoch
Right ascension17h 47m 20.4s[1]
Declination−28° 23′ 07″[1]
ConstellationSagittarius
Physical characteristics
Radius23 pc
DesignationsSagittarius B2, Sgr B2
See also: Lists of nebulae

Sagittarius B2 (Sgr B2) is a giant molecular cloud of gas and dust that is located about 120 parsecs (390 ly) from the center of the Milky Way. This complex is the largest molecular cloud in the vicinity of the core and one of the largest in the galaxy, spanning a region about 45 parsecs (150 ly) across.[2] The total mass of Sgr B2 is about 3 million times the mass of the Sun.[3] The mean hydrogen density within the cloud is 3000 atoms per cm3, which is about 20–40 times denser than a typical molecular cloud.[4]

The internal structure of this cloud is complex, with varying densities and temperatures. The cloud is divided into three main cores, designated north (N), middle or main (M) and south (S) respectively. Thus Sgr B2(N) represents the north core. The sites Sgr B2(M) and Sgr B2(N) are sites of prolific star formation. The first 10 H II regions discovered were designated A through J.[5] H II regions A–G, I and J lie within Sgr B2(M), while region K is in Sgr B2(N) and region H is in Sgr B2(S).[6] The 5-parsec-wide core of the cloud is a star-forming region that is emitting about 10 million times the luminosity of the Sun.[7]

The cloud is composed of various kinds of complex molecules, of particular interest: alcohol. The cloud contains ethanol, vinyl alcohol, and methanol. This is due to the conglomeration of atoms resulting in new molecules. The composition was discovered via spectrograph in an attempt to discover amino acids. An ester, ethyl formate, was also discovered, which is a major precursor to amino acids. This ester is also responsible for the flavour of raspberries,[8] leading some articles on Sagittarius B2 to postulate the cloud as smelling of ‘raspberry rum’.[9][10] Large quantities of butyronitrile (propyl cyanide) and other alkyl cyanides have also been detected as being present in the cloud.[11]

Temperatures in the cloud vary from 300 K (27 °C) in dense star-forming regions to 40 K (−233.2 °C) in the surrounding envelope.[12] Because the average temperature and pressure in Sgr B2 are low, chemistry based on the direct interaction of atoms is exceedingly slow. However, the Sgr B2 complex contains cold dust grains consisting of a silicon core surrounded by a mantle of water ice and various carbon compounds. The surfaces of these grains allow chemical reactions to occur by accreting molecules that can then interact with neighboring compounds. The resulting compounds can then evaporate from the surface and join the molecular cloud.[2]

The molecular components of this cloud can be readily observed in the 102–103 μm range of wavelengths.[2] About half of all the known interstellar molecules were first found near Sgr B2, and nearly every other currently known molecule has since been detected in this feature.[13]

The European Space Agency's gamma-ray observatory INTEGRAL has observed gamma rays interacting with Sgr B2, causing X-ray emission from the molecular cloud. This energy was emitted about 350 years prior by the supermassive black hole (SMBH) at the galaxy's core, Sagittarius A*. The total luminosity from this outburst is an estimated million times stronger than the current output from Sagittarius A*.[14][15] This conclusion was supported in 2011 by Japanese astronomers who observed the Galactic Center with the Suzaku satellite.[16]

Observations with the James Webb Space Telescope revealed new candidate HII regions that were missed with radio observations. At 25 μm the researchers found infrared radiation escaping the protocluster Sgr B2 N, following the path of a large-scale outflow. YSOs previously detected with ALMA in the western side of the cloud are not detected with JWST, but hot dust around their outflows is detected with JWST. On the eastern side JWST detects recent star-formation.[17]

[edit]
  • Sagittarius B2 is seen here the right orange-red region to the middle left of the image. Image by ATLASGAL (red) and MSX (blue, green).
    Sagittarius B2 is seen here the right orange-red region to the middle left of the image. Image by ATLASGAL (red) and MSX (blue, green).
  • JWST NIRCam image of star-formation in Sagittarius B2.
    JWST NIRCam image of star-formation in Sagittarius B2.

See also

[edit]

References

[edit]
[edit]
Revisions and contributorsEdit on WikipediaRead on Wikipedia

Sagittarius B2

View on Grokipedia
from Grokipedia
Sagittarius B2 (Sgr B2) is the most massive molecular cloud complex in the Milky Way, located near the center of the galaxy, approximately 26,000–27,000 light-years from Earth in the constellation Sagittarius. It represents the galaxy's largest and most active star-forming region, spanning roughly 30–45 parsecs (about 100–150 light-years) across and containing a total gas mass of around 8 × 10⁶ solar masses. This dense agglomeration of interstellar gas and dust is renowned for its extraordinary chemical richness, harboring a large number of complex organic molecules including over 50 detected species, and serves as a key laboratory for studying high-mass star formation and galactic center dynamics. Positioned just a few hundred light-years from Sagittarius A*, the at the Milky Way's core, Sgr B2 is situated at a precise of 8.34 ± 0.16 kiloparsecs from the Sun. Despite comprising only about 10% of the galactic center's total gas reservoir, it accounts for roughly 50% of the stars formed in that region, with an estimated rate of 0.01–0.04 solar masses per year. The complex features prominent subregions, such as Sgr B2(N) and Sgr B2(M), which host clusters of young, massive stars embedded in hot cores and H II regions, driving intense radiative and mechanical feedback that shapes the cloud's evolution. Observations by the (JWST) released in 2025 have provided unprecedented views of Sgr B2, using its NIRCam and instruments to penetrate the thick dust and reveal glowing warm dust grains heated by embedded protostars, as well as dense, opaque cores that obscure even infrared light and signal sites of future star birth. These insights highlight Sgr B2's role in producing half the stellar output of the , underscoring its significance in understanding the processes that fuel galaxy-wide amid extreme environmental conditions.

Location and Overview

Position and Distance

Sagittarius B2 is situated near the , with galactic coordinates of ℓ = 0.67°, b = −0.04° and equatorial coordinates of RA 17ʰ 47ᵐ 20.⁴ˢ, Dec −28° 22′ 07″ (J2000.0). These positions place it within the central molecular zone of the , approximately 120 parsecs (390 light-years) from Sagittarius A*, the at the . The cloud complex lies at a distance of approximately 8.3 kiloparsecs (27,000 light-years) from the Solar System, making it one of the closest massive star-forming regions to the galactic nucleus. The to Sagittarius B2 has been determined primarily through trigonometric measurements using (VLBI) observations of associated water masers. Early VLBI efforts yielded a of 0.129 ± 0.012 mas, corresponding to a of 7.9^{+0.8}_{-0.7} kpc, with subsequent analyses this to 8.34 ± 0.16 kpc, consistent with the . These measurements also incorporate comparisons with proper motions relative to other features in the Sagittarius B complex, confirming its orbital alignment and proximity to the . As part of the larger , Sagittarius B2 represents a key component of the dense gas environment surrounding the , spanning several parsecs and influencing the dynamics of nearby . This positioning underscores its role in probing the extreme conditions near the Milky Way's core.

Discovery and Initial Observations

Sagittarius B2 was first identified as a dense through radio observations of (NH₃) inversion lines in 1968, when Cheung et al. detected emission from the (J,K)=(1,1) transition toward the region, marking one of the earliest confirmations of polyatomic molecules in a compact interstellar source. This discovery highlighted Sgr B2's high density, with estimated values exceeding 10⁵ cm⁻³ based on the excitation of the lines, distinguishing it from more diffuse clouds. Subsequent follow-up observations in 1973 by Morris et al. refined these findings, mapping the spatial extent of NH₃ emission over several arcminutes and confirming the cloud's thermalized conditions indicative of dense, warm gas. In the 1980s, initial mapping efforts using millimeter-wave telescopes revealed Sgr B2 as a giant complex spanning tens of parsecs, with extensive surveys of rotational transitions from species like CO and HCN showing structured emission peaks aligned with embedded sources. These observations, conducted with instruments such as the Bell Laboratories 7 m telescope, covered frequencies from 70 to 150 GHz and uncovered over 100 spectral lines, delineating the cloud's overall morphology and velocity gradients suggestive of internal dynamics. The proximity of Sgr B2 to the , approximately 100 pc away, further motivated these early studies due to its potential insights into central molecular zone processes. Early evidence of active in Sgr B2 emerged from detections of radio recombination lines (RRLs) in the 1970s, which indicated the presence of ionized regions (H II regions) excited by massive young stars. Observations of and RRLs, such as H76α and He76α, showed line widths consistent with thermal broadening in ultracompact H II regions, providing the first spectroscopic confirmation of ongoing high-mass within the cloud. By the , Sgr B2 had become recognized as a premier astrochemical laboratory, serving as the site for the first detections of numerous complex organic molecules through targeted millimeter and submillimeter surveys that revealed rich spectral forests. Seminal work by Turner identified species like and other organics, underscoring the cloud's role in testing models of interstellar synthesis pathways under dense, irradiated conditions.

Physical Structure

Size, Mass, and Density

Sagittarius B2 is one of the largest and most massive molecular clouds in the , extending across a of approximately 45 parsecs, or about 150 light-years, with a corresponding radius of roughly 23 parsecs. This physical extent is determined through three-dimensional modeling of thermal dust emission, encompassing scales from subparsec cores to the overall cloud envelope. The cloud's structure is filamentary, converging toward a central hub, which contributes to its overall . The total mass of Sagittarius B2 is estimated at around 8 × 10⁶ solar masses (M⊙), primarily derived from dust continuum modeling and CO emission line observations that trace the gas distribution across the . This mass is predominantly contained within the outer envelope, which accounts for over 99% of the total, while the inner regions host denser concentrations. estimates, calculated using the applied to linewidths and cloud dimensions, yield values consistent with this total mass, indicating dynamical stability against on large scales. The division into northern, main, and southern cores influences the mass distribution, with the harboring a significant fraction of the overall material. The mean density in the envelope is approximately 3000 atoms per cm³, reflecting the typical conditions in the outer layers of the cloud, while densities increase dramatically to greater than 10⁶ cm⁻³ in the embedded dense cores. This density profile follows a Plummer-like distribution in the inner regions, transitioning to lower values outward, as inferred from multi-wavelength continuum data. The temperature profile varies radially, with the envelope maintaining temperatures around 40 due to shielding from interstellar radiation, rising to about 300 in the inner hot regions heated by embedded activity.

Internal Cores and Subregions

Sagittarius B2 is subdivided into three primary internal cores—Sgr B2(N) in the north, Sgr B2(M) in the central region, and Sgr B2(S) in the south—each representing distinct structural and evolutionary components within the overall cloud complex, which encompasses a total gas mass of approximately 8 × 10^6 M_⊙. These cores exhibit significant density contrasts, with peak H_2 densities reaching up to ~10^9 cm^{-3} in their innermost regions, embedding clusters of massive stars that drive local dynamics. The subdivision reflects an evolutionary sequence from a more quiescent outer envelope to increasingly active inner cores, influencing the cloud's overall and fragmentation. Sgr B2(N) is the northern core and is at an intermediate evolutionary stage, characterized by its high level of activity, hosting eight ultra-compact H II (UCH II) regions with sizes ranging from 0.006 to 0.04 pc and electron densities of ~10^4 to ~10^6 cm^{-3}. Surrounding dense gas reaches densities of ~10^6–10^9 cm^{-3}, supporting embedded massive star clusters that contribute to the core's dynamic structure. This core's properties indicate ongoing intense processes transitioning from envelope-like quiescence to more evolved states. The central core, Sgr B2(M), is the main and most luminous component, with a total luminosity of ~1.2 × 10^7 L_⊙, marking it as the most evolved of the subregions and containing 40 UCH II regions of similar sizes (0.006–0.04 pc) and densities (~10^4–10^6 cm^{-3}). Its high density peaks and extensive embedded massive star clusters underscore a mature structural configuration, with dense gas at ~10^6–10^9 cm^{-3} enhancing the core's stability and activity. Sgr B2(S), the southern core, is the least evolved, featuring only two UCH II regions with comparable sizes and electron densities to those in the northern and central cores, alongside lower overall activity indicative of an earlier stage in the evolutionary progression from the quiescent envelope. Dense gas densities here also span ~10^6–10^9 cm^{-3}, but with fewer embedded massive stars, reflecting a transitional structure less influenced by advanced dynamical processes. These cores contain numerous substructures, including H II regions often labeled A through J in early mappings, with representative sizes of ~0.1 pc and electron densities around 10^4–10^5 cm^{-3}, contributing to the cloud's compartmentalized density profile. The interplay between these subregions and the surrounding drives the cloud's evolution, with higher densities in the cores fostering localized clustering of massive stars.

Chemical Composition

Interstellar Molecules

Sagittarius B2 harbors one of the richest known inventories of interstellar molecules, with dozens to over 100 distinct species and their isotopologs detected through extensive radio surveys, underscoring its significance in astrochemical research. Approximately half of all known interstellar molecules were first identified in this region, highlighting its role as a primary laboratory for molecular complexity in the interstellar medium. Key detections include simple alcohols such as methanol (CH3OHCH_3OH), ethanol (C2H5OHC_2H_5OH), vinyl alcohol (CH2CHOHCH_2CHOH), and more recent findings like iso-propanol (CH3CH(OH)CH3CH_3CH(OH)CH_3) (as of 2022), as well as complex organics like ethyl formate (C2H5OCHOC_2H_5OCHO), butyronitrile (C3H7CNC_3H_7CN), propionamide (C2H5CONH2C_2H_5CONH_2) (as of 2022), and various alkyl cyanides (e.g., iso-propyl cyanide, i−C3H7CNi-C_3H_7CN). These molecules span inorganic species like carbon monoxide (COCO) and ammonia (NH3NH_3) to prebiotic-relevant organics, with detections spanning millimeter to submillimeter wavelengths. Abundance profiles reveal that complex organic molecules in Sagittarius B2 typically reach levels of ∼10−8\sim 10^{-8} relative to H2H_2, establishing the region as a benchmark for high molecular densities in star-forming environments. For example, iso-propyl exhibits an abundance of ∼8×10−9\sim 8 \times 10^{-9} toward Sgr B2(N), while normal-propyl is around 3.6×10−93.6 \times 10^{-9}. Variations exist across subregions; cyanides and nitriles are notably more abundant in the northern core (Sgr B2(N)), with column densities up to 101710^{17} cm−2^{-2}, compared to the main core (Sgr B2(M)), where sulfur-bearing species dominate. These profiles reflect and gradients, with hotter cores favoring volatile release and enhanced synthesis. The formation of these molecules proceeds via gas-phase ion-molecule reactions and surface chemistry on dust s, where atomic and radical species accrete and recombine under varying temperatures. In cold phases (∼10\sim 10 K), radical diffusion on icy grain mantles builds complex organics like alcohols and esters; subsequent warm-up (>100>100 K) desorbs them into the gas phase. Cosmic-ray-induced photolysis further drives radical production, enabling pathways such as insertion into hydrocarbons to form nitriles. Isotopic ratios provide insights into nucleosynthetic enrichment; the 12^{12}C/13^{13}C ratio in Sgr B2 ranges from 15 to 33 (average 24±724 \pm 7), lower than the solar value of 89, signaling 13^{13}C enhancement from stellar processing.

Dust Grains and Mantles

In Sagittarius B2, the dust grains primarily consist of cores coated with carbonaceous mantles, a composition typical of interstellar in dense molecular clouds. These grains exhibit opacity at millimeter wavelengths ranging from approximately 0.1 to 1 cm²/g, influencing the observed continuum emission in radio observations of the region. This opacity arises from the combined absorption and scattering properties of the and carbon components, with values derived from models of agglomerated grains in dense environments. The ice mantles surrounding these dust grains in the colder regions of Sagittarius B2 are dominated by water ice (H₂O), with significant contributions from CO, CO₂, and (CH₃OH) ices. These mantles can reach thicknesses of up to 100–160 monolayers after extended periods of growth in dense, cold conditions (T ≤ 15 K). Dust grain surfaces in Sagittarius B2 play a crucial catalytic role in interstellar chemistry, facilitating reactions (e.g., CO to CH₃OH) and radical recombination processes that lead to the formation of complex organic molecules. These surface-mediated pathways are essential in the cold phases, where gas-phase reactions are inefficient due to low temperatures and densities. As temperatures rise above 100 K in the hot cores of Sagittarius B2, the ice mantles undergo thermal desorption, evaporating volatiles such as H₂O, CO, CO₂, and into the gas phase and altering the chemical inventory of the surrounding environment. This process, occurring around 120–147 K for key species like , releases surface-synthesized molecules and enables subsequent gas-phase reactions.

Star Formation Activity

Hot Cores and HII Regions

Sagittarius B2 hosts numerous hot cores, which are compact, dense regions of gas and heated to temperatures exceeding 100 K by embedded massive protostars. These structures, typically spanning about 0.1 pc, arise from the of fragments, where protostellar heating causes the sublimation of mantles on grains, releasing complex molecules into the gas phase. In Sgr B2(N) and Sgr B2(M), ALMA observations have identified 47 such hot cores, with temperatures ranging from 190 K to 342 K, and peak temperatures in some reaching up to 662 K in the Deep South region. The hot cores exhibit heterogeneous thermal profiles, often modeled with broken power laws, reflecting varying stages of high-mass within the cloud's internal subregions. Adjacent to these hot cores are H II regions, ionized zones created by radiation from O and B-type stars that ionize surrounding gas, forming expanding fronts. In Sagittarius B2, these regions are labeled A through J, primarily located within Sgr B2(M), with additional ones in Sgr B2(N) and Sgr B2(S); they produce radio free-free emission detectable at centimeter wavelengths. The H II regions vary in size from hyper-compact scales of 10–200 AU for the youngest ultra-compact variants to larger structures up to 2 pc, with electron densities around 10^7 cm⁻³ and electron temperatures typically between 5000 K and 9000 K. Their formation follows the maturation of hot cores, as massive stars emerge and begin ionizing their natal envelopes, with dynamical ages estimated at 3000–7000 years for select regions based on expansion models. Collectively, the hot cores and H II regions in Sagittarius B2 contribute significantly to the complex's total , estimated at around 10^7 L_⊙, primarily from Sgr B2(N) and Sgr B2(M) at 2–10 × 10^6 L_⊙ each. This intense activity drives outflows and interactions that shape the surrounding medium, enhancing the region's role as a prolific site of high-mass near the . Observations reveal dynamical interactions, such as outflows from protostars influencing nearby fronts, underscoring the evolutionary linkage between these thermal and ionized structures.

Young Stellar Objects and Protostars

Sagittarius B2 hosts a rich population of young stellar objects (YSOs), primarily in the form of Class 0 and Class I protostars embedded within its dense molecular cores. Previous ALMA observations have identified over 700 YSOs across the complex, with a significant fraction consisting of high-mass protostellar cores; specifically, 271 such cores were detected at 3 mm wavelengths, many exhibiting infrared excess indicative of active accretion disks. These protostars are predominantly massive, with estimated stellar masses ranging from 8 to 20 M⊙ for the high-mass examples, reflecting the region's capacity for forming stars far exceeding solar mass. Embedded clusters are prominent in subregions like Sgr B2(M), where the (IMF) shows a toward high-mass stars, consistent with an excess of massive protostars relative to lower-mass counterparts. Accretion processes in these protostars occur at rates around 10^{-3} M_⊙ yr^{-1} during early phases, enabling rapid growth despite the intense radiation pressures involved. These clusters, including those in Sgr B2(N) and Sgr B2(S), represent protoclusters in various evolutionary stages, with Sgr B2(M) displaying more evolved embedded populations. Recent observations, as of September 2025, have provided high-resolution infrared views of these YSOs and protostars, revealing outflow cavities that allow 25 μm emission to escape dense envelopes in Sgr B2(N) and confirming the absence of an extended low-mass YSO , which supports the high-mass bias. These images highlight the role of feedback from massive protostars in dispersing and regulating further collapse. Bipolar outflows and jets from these protostars are widespread, extending up to 1 pc in length and driving significant dynamical activity within the cloud. These outflows are traced by molecular emissions such as SiO and H_2O s, with hundreds of maser sites associated with protostellar cores and outflows across Sgr B2. The feedback from these YSOs, including outflow-induced shocks and turbulence, plays a key role in regulating the cloud's evolution by dispersing , injecting momentum, and potentially triggering subsequent in surrounding dense regions.

Observational History

Early Radio and Spectroscopic Studies

The initial detection of Sagittarius B2 as a dense molecular cloud came from observations of ammonia (NH3) inversion lines in the 1970s, revealing its location near the Galactic center and highlighting its richness in molecular species. Systematic radio and spectroscopic studies in the 1980s and 1990s focused on mapping the cloud's structure and chemistry using millimeter-wave observations. Key surveys with the Berkeley-Illinois-Maryland Association (BIMA) array targeted tracers like carbon monoxide (CO) and ammonia (NH3), achieving resolutions of 1–5 arcseconds to resolve internal cores. For instance, BIMA mappings of the CO J=1–0 transition at 115 GHz delineated the extent of the molecular envelope, showing extended emission over several parsecs with velocity gradients indicative of rotation or infall. Similarly, NH3 observations, including metastable (J,K)=(3,3) and non-metastable transitions, revealed compact hot core regions with temperatures exceeding 100 K, distinguishing Sgr B2's substructures from the surrounding Galactic center material. Single-dish telescopes, such as the National Radio Astronomy Observatory (NRAO) 12 m dish, conducted extensive molecular line surveys that detected over 20 species, including rotational transitions like CO J=1–0 at 115 GHz and various isotopologues. These surveys identified complex organics like (CH3OH) and (HCN), establishing Sgr B2 as a chemically diverse region with line widths broadened by and outflows. Dust continuum measurements complemented these efforts; early submillimeter photometry at 1.3 mm with the James Clerk Maxwell Telescope estimated the cloud's total mass at around 10^4 solar masses, assuming optically thin emission from warm dust grains at temperatures of 20–40 K. Challenges in these early studies arose from foreground confusion due to the dense environment, which superimposed unrelated emission along the . This was mitigated through multi-line fitting techniques, comparing profiles of multiple and isotopologues to disentangle components and derive accurate column densities. Such methods confirmed the dominance of Sgr B2's emission at velocities around 60–70 km/s, separating it from intervening clouds.

Modern Infrared and X-ray Observations

In the 2010s, the Herschel Space Observatory's Heterodyne Instrument for the (HIFI) conducted a comprehensive survey of Sagittarius B2, targeting both the Main (Sgr B2(M)) and Northern (Sgr B2(N)) cores. This effort detected over 100 molecular transitions across the far-infrared spectrum, enabling detailed modeling of excitation temperatures that ranged from cold envelope conditions around 5–14 to warmer hot core environments exceeding 100 . Observations from the in the 2000s provided evidence of a past outburst from the Sagittarius A*, whose high-energy radiation illuminated Sagittarius B2 approximately 350 years ago. The gamma-ray data revealed interactions producing fluorescent X-ray emission in the , with the delayed signal consistent with the light-travel time across the ~100 pc distance from the . Suzaku X-ray observations in 2009 mapped diffuse emission from hot plasma enveloping Sagittarius B2, indicating temperatures around 10^7 K and suggesting an extension of the Galactic center's thermal plasma into the region. This emission, characterized by iron K-shell lines at ~6.4 keV from neutral material and broader lines from ionized gas, highlighted the cloud's interaction with pervasive hot diffuse gas. The (JWST), utilizing its Near-Infrared Camera (NIRCam) and (MIRI) in 2025, delivered high-resolution images of Sagittarius B2, particularly Sgr B2(N), revealing intricate dust lanes, newly identified H II regions, and young stellar objects (YSOs) resolved down to 0.1 pc scales. spectroscopy at 25 μm prominently featured polycyclic aromatic hydrocarbon (PAH) emission bands, underscoring active amid warm dust and ionized gas structures. Recent Atacama Large Millimeter/submillimeter Array (ALMA) reanalyses of Sagittarius B2's core spectra have refined physical and chemical models by incorporating multi-line data and dust attenuation effects, leading to abundance revisions for key molecules by factors of 2–5 compared to earlier single-line estimates. These updates, derived from unbiased Band 6 surveys covering 211–275 GHz, enhance understanding of hot core evolution without altering foundational radio baselines from prior decades.

References

  1. https://www.aanda.org/articles/aa/full_html/2016/04/aa27311-15/aa27311-15.html
  2. https://www.aanda.org/articles/aa/full_html/2019/08/aa35200-19/aa35200-19.html
  3. https://science.[nasa](/page/NASA).gov/missions/webb/nasas-webb-explores-largest-star-forming-cloud-in-milky-way/
  4. https://esawebb.org/news/weic2520/
  5. https://science.nasa.gov/missions/webb/nasas-webb-explores-largest-star-forming-cloud-in-milky-way/
  6. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Sagittarius+B2
  7. https://iopscience.iop.org/article/10.1088/0004-637X/705/2/1548
  8. https://arxiv.org/pdf/1401.5377
  9. https://arxiv.org/abs/0908.3637
  10. https://www.aanda.org/articles/aa/full_html/2023/08/aa46903-23/aa46903-23.html
  11. https://ui.adsabs.harvard.edu/abs/1968PhRvL..21.1701C
  12. https://ui.adsabs.harvard.edu/abs/1973ApJ...186..501M/abstract
  13. https://www.aanda.org/articles/aa/full_html/2022/10/aa43674-22/aa43674-22.html
  14. https://www.aanda.org/articles/aa/full_html/2025/01/aa51274-24/aa51274-24.html
  15. https://www.aanda.org/articles/aa/full_html/2011/06/aa16928-11/aa16928-11.html
  16. https://pmc.ncbi.nlm.nih.gov/articles/PMC1567865/
  17. https://ui.adsabs.harvard.edu/abs/2013A&A...559A..47B/abstract
  18. https://www.science.org/doi/10.1126/science.aae0328
  19. https://www.sci.news/astronomy/alma-interstellar-propanol-its-isomer-milky-ways-center-10966.html
  20. https://iopscience.iop.org/article/10.3847/1538-4357/ac8668
  21. https://www.mpia.de/4794999/Garrod.pdf
  22. https://arxiv.org/abs/1906.04695
  23. https://phys.org/news/2016-06-life-handshake-chiral-molecule-interstellar.html
  24. https://iopscience.iop.org/article/10.3847/1538-4357/aa816b
  25. https://arxiv.org/pdf/astro-ph/0304489
  26. https://www.aanda.org/articles/aa/full_html/2017/08/aa30426-17/aa30426-17.html
  27. https://www.aanda.org/articles/aa/pdf/2019/08/aa35523-19.pdf
  28. https://doi.org/10.1051/0004-6361/202346903
  29. https://iopscience.iop.org/article/10.3847/1538-4357/ad1507
  30. https://iopscience.iop.org/article/10.3847/1538-4357/ad0383
  31. https://www.aanda.org/articles/aa/full_html/2019/08/aa35523-19/aa35523-19.html
  32. https://arxiv.org/pdf/2509.11771
  33. https://arxiv.org/abs/2509.11771
  34. https://iopscience.iop.org/article/10.3847/1538-4357/adea3b
  35. https://ui.adsabs.harvard.edu/abs/1995ApJ...454..782M/abstract
  36. https://ui.adsabs.harvard.edu/abs/1989ApJS...70..539T/abstract
  37. https://www.aanda.org/articles/aa/full_html/2021/07/aa40203-20/aa40203-20.html
  38. https://iopscience.iop.org/article/10.1088/0004-637X/789/1/8
  39. https://iopscience.iop.org/article/10.1086/422487
  40. https://academic.oup.com/pasj/article/61/4/751/1539333
  41. https://academic.oup.com/pasj/article/60/sp1/S191/1460421
  42. https://www.aanda.org/articles/aa/abs/2025/01/aa51274-24/aa51274-24.html
  43. https://arxiv.org/pdf/2307.06222
Add your contribution
Related Hubs
User Avatar
No comments yet.