Identification of interstellar cyanamide towards the hot molecular core G358.93–0.03 MM1

Detection and Chemical Modeling of Complex Prebiotic Molecule Cyanamide in the Hot Molecular Core G31.41 + 0.31

“…It shows NH 2 CN is created toward G31.41 + 0.31 via the neutral–neutral reaction between NH 2 and CN on the grain surface of the hot core. Recently, Manna and Pal determined that the fractional abundance of NH 2 CN toward another hot molecular core, G358.93 – 0.03 MM1, is (4.72 ± 2.0) × 10 –10 , which is similar to the modeled abundance of NH 2 CN. This indicates that, like G31.41 + 0.31, NH 2 CN is created via the neutral–neutral reaction between NH 2 and CN on the grain surface toward the other hot molecular core, G358.93 – 0.03 MM1.…”

“…Here, we compare the derived fractional abundance of NH 2 CN in G31.41 + 0.31 with other hot molecular cores and hot corino objects. Previously, the rotational emission lines of NH 2 CN were detected in hot molecular cores Sgr B2 (M), Sgr B2 (N), IRAS 20126 + 4104, G10.47 + 0.03, and G358.93 – 0.03 MM1, with estimated fractional abundances of 3.54 × 10 –12 , 5.13 × 10 –9 , 1.2 × 10 –9 , 5.07 × 10 –8 , and (4.72 ± 2.0) × 10 –10 , respectively. ,− , Similarly, the fractional abundances of NH 2 CN toward the hot corino objects NGC 1333 IRAS4A2, NGC 1333 IRAS2A, and IRAS 16293-2422 B were 1.7 × 10 –10 , 5.0 × 10 –11 , and 2.0 × 10 –10 , respectively. , We estimate that the fractional abundance of NH 2 CN toward the G31.41 + 0.31 is (7.21 ± 1.46) × 10 –10 . This comparison indicates that the abundance of NH 2 CN in the hot core G31.41 + 0.31 is similar to that of the hot core G358.93 – 0.03 MM1 and the hot corinos NGC 1333 IRAS4A2 and IRAS 16293-2422 B.…”

“…The full width at half-maximum (FWHM) of the LTE spectra of NH 2 CN is 5.2 ± 0.8 km s −1 . Our estimated excitation temperature shows that the detected transition lines of NH 2 CN arise from the warm inner region of G31.41 + 0.31 because the temperature of the hot molecular cores exceeds 100 K. 21 We also searched for rotational emission lines of NH 2 13 CN and NH 2 C 15 N in the molecular spectra of G31.41 + 0.31 using the LTE model, but we could not detect these molecules. The upper limit column densities of NH 2 13 CN and NH 2 C 15 N are ≤3.2 × 10 13 and ≤5.8 × 10 13 cm −2 .…”

“…14,23,24 Earlier, Manna and Pal, 13 Coutens et al, 14 Garrod, 23 Garrod and Herbst, 24 and Garrod et al 25 claimed reaction 1 is the most efficient way to produce NH 2 CN on the grain surface of hot molecular cores and hot corinos. Previously, Manna & Pal 13 and Coutens et al 14 showed reaction 1 is responsible for the production of NH 2 CN toward the hot core G358.93 − 0.03 MM1 and the hot corino IRAS 16293 B. We claim that reaction 1 may be efficient for the formation of NH 2 CN toward G31.41 + 0.31 because the parent molecule NH 2 produces NH 3 by radical recombination with hydrogen atoms and NH 2 or by hydrogen abstraction from H 2 molecules, 24 and previously Cesaroni et al 45 detected the rotational emission lines of NH 3 from G31.41 + 0.31 and other hot cores.…”

“…The magnetic dipole moments of the 0 – and 0 + substates are 4.24 and 4.25 debye, respectively . The emission lines of NH 2 CN were detected in the hot molecular cores Sgr B2 (N), , Sgr B2 (M), IRAS 20126 + 410, Orion KL, G10.47 + 0.03, G358.93 – 0.03 MM1, solar-like protostars IRAS 16293 – 2422 B and NGC 1333 IRAS2A, starburst galaxy M82, and sculptor galaxy NGC 253 …”