Complex organic molecules (COMs) have been detected ubiquitously in protostellar systems. However, at shorter wavelengths (~0.8mm) it is more difficult to detect larger molecules than at longer wavelengths (~3mm) because […]
Interstellar
Posted inAstrochemistry, Astronomy & Telescopes, Interstellar, Status Report
Organic Chemistry In The H2-bearing, CO-rich Interstellar Ice Layer At Temperatures Relevant To Dense Cloud Interiors
Ice chemistry in the dense, cold interstellar medium (ISM) is probably responsible for the formation of interstellar complex organic molecules (COMs).
![Overview of the d203-506 externally irradiated protoplanetary disk. Integrated intensity images from NIRCam F212N filter (a), Hubble Space Telescope [OI] (b), NIRSpec [FeII] (c), NIRSpec CH+ 1-0 P(7) at 3.95 µm (d), and MIRI MRS integrated from 7.16 to 7.20 µm assigned to CH+ 3 (e). Each panel is centered at α=5:35:20.318 and δ=-5:25:05.662 and are 2" × 2" wide. Contours of NIRCam vibrationally excited H2 (2.12 µm band) are represented in orange, and ALMA dust continuum emission at 344 GHz from the disk in white contours. (f,) Sketch of the d203-506 disk, jet, and wind. We note that the low mass star is not seen in the images because of the disk flaring. All JWST images are from the PDRs4All program, while the Hubble image is from (9). -- astro-ph.GA](https://i0.wp.com/astrobiology.com/wp-content/uploads/2024/01/FormationoftheMethylCation.png?resize=1200%2C719&ssl=1)
Posted inAstrochemistry, Astronomy & Telescopes, Biochemistry & Organic Chemistry, Interstellar, Status Report
Formation Of The Methyl Cation By Photochemistry In A Protoplanetary Disk
Forty years ago it was proposed that gas phase organic chemistry in the interstellar medium was initiated by the methyl cation CH3+, but hitherto it has not been observed outside […]
Posted inAstrochemistry, Astrogeology, Astronomy & Telescopes, Interstellar, Status Report
Water Transport Through Mesoporous Amorphous-carbon Dust
The diffusion of water molecules through mesoporous dust of amorphous carbon (a-C) is a key process in the evolution of prestellar, protostellar, and protoplanetary dust, as well as in that […]
Posted inAstrochemistry, Astronomy & Telescopes, Imaging & Spectroscopy, Interstellar, Status Report
Structures Of Dust and gAs (SODA): Constraining The Innermost Dust Properties of II Zw96 With JWST Observations Of H2O And CO
We analyze JWST NIRSpec+MIRI/MRS observations of the infrared (IR) gas-phase molecular bands of the most enshrouded source (D1) within the interacting system and luminous IR galaxy II Zw 096.
Posted inAstrogeology, Astronomy & Telescopes, Biosignatures & Paleobiology, Comets and Asteroids, Interstellar, Origin & Evolution of Life, Panspermia, Planetary Protection & Biosafety, Status Report
The Implications Of ‘Oumuamua On Panspermia
Panspermia is the hypothesis that life originated on Earth from the bombardment of foreign interstellar ejecta harboring polyextremophile microorganisms.
Posted inAstrochemistry, Astronomy & Telescopes, Biochemistry & Organic Chemistry, Biosignatures & Paleobiology, Imaging & Spectroscopy, Interstellar, Press Release
R Leporis – Surrounded By A Cloud Of Carbon Compounds – As Imaged By ALMA
The Atacama Large Millimeter/submillimeter Array (ALMA), in which ESO is a partner, has achieved the highest resolution observations since it began operations.
Posted inAstronomy & Telescopes, Budgets and Policy, Conferences and Meetings, Intelligence & Language, Interstellar, SETI & Technosignatures, Societal Issues, Status Report
Bio-techno-signature Monitoring and Communication Guideposts for Extraterrestrial Life
Abstract — Attendees at the First Penn State SETI Symposium collaborated to develop guideposts for monitoring for and communicating with extraterrestrial life.
![JWST NIRCam composite image of the Orion Bar, located in the Orion molecular cloud. Red is the 3.35µm emission (F335M NIRCam filter), blue is the emission of Paα (F187N filter subtracted by F182M filter) and green is the emission of the H2 0-0 S(9) line at 4.70 µm (F470N filter subtracted by F480M filter). The inset shows a zoom-in of the d203-506 planet-forming disk where OH lines are detected. Red is the emission of the H2 1-0 S(1) line at 2.12 µm (F212N filter), blue is the [FeII] line emission at 1.64 µm (F164N filter), and green is the emission in the F140M broad-band near-IR filter that traces scattered light around 1.4 µm (F140M broad band filter). The white contours represent the emission of the OH rotational line at 9.79 µm detected with MIRI-MRS (levels are 1.1, 2.5 ×10−5 erg cm−2 s −1 sr−1 ). The bright spot in the northwestern part of the envelope coincides with the region of interaction between a jet and the photoevaporative wind. The brightest OH emission originates from here. The spectra shown in Fig. 2 and 3 are an average over the region delineated by the green circle in order to have the best S/N. Image credits: NASA, ESA, CSA, PDRs4All ERS Team, pdrs4all.org. -- astro-ph.EP](https://i0.wp.com/astrobiology.com/wp-content/uploads/2023/12/OHAsAProbe.png?resize=1200%2C717&ssl=1)
Posted inAstrochemistry, Astronomy & Telescopes, Biochemistry & Organic Chemistry, Biosignatures & Paleobiology, Habitable Zones, Icy Worlds, Interstellar, Status Report, Water/Hycean Worlds & Oceanography
OH As A Probe Of The Warm Water Cycle In Planet-forming Disks
Water is a key ingredient for the emergence of life as we know it. Yet, its destruction and reformation in space remains unprobed in warm gas.
Posted inAstrogeology, Biochemistry & Organic Chemistry, Biosignatures & Paleobiology, Imaging & Spectroscopy, Interstellar, Status Report
Synthesis Of Urea On The Surface Of Interstellar Water Ice Clusters. A Quantum Chemical Study
Urea is a prebiotic molecule that has been detected in few sources of the interstellar medium (ISM) and in Murchison meteorite. Being stable against ultraviolet radiation and high-energy electron bombardment, […]