The Submillimeter Spectrum of the Orion Star Forming Region Mary L. Radhuber, Jay A. Kroll, Susanna L. Widicus Weaver Department of Chemistry Emory University

Why Line Surveys? Large swaths of frequency covered in single observations More observed transitions leads to better identification certainty. Large amounts of data are acquired in short amounts of time. Similar instrument and calibration conditions for an entire observation Better internal consistency of intensity measurements leads to a more accurate measurement of physical conditions.

2 atoms3 atoms4 atoms5 atoms6 atoms7 atoms8 atoms9 atoms10 atoms11 atoms12 atoms13 atoms H2H2 C3C3 c-C 3 HC5C5 C5HC5HC6HC6HCH 3 C 3 NCH 3 C 4 HCH 3 C 5 NHC 9 NC6H6C6H6 HC 11 N AlFC2HC2Hl-C 3 HC4HC4Hl-H 2 C 4 CH 2 CHCNHC(O)OCH 3 CH 3 CH 2 CN(CH 3 ) 2 COCH 3 C 6 HC 2 H 5 OCH 3 AlClC2OC2OC3NC3NC 4 SiC2H4C2H4 CH 3 C 2 HCH 3 COOH(CH 3 ) 2 O(CH 2 OH) 2 C2C2 C2SC2SC3OC3Ol-C 3 H 2 CH 3 CNHC 5 NC7HC7HCH 3 CH 2 OHCH 3 CH 2 CHO CHCH 2 C3SC3Sc-C 3 H 2 CH 3 NCCH 3 CHOH2C6H2C6 HC 7 N CH + HCNC2H2C2H2 H 2 CCNCH 3 OHCH 3 NH 2 CH 2 OHCHOC8HC8H CNHCONH 3 CH 4 CH 3 SHc-C 2 H 4 Ol-HC 6 HCH 3 C(O)NH 2 COHCO + HCCNHC 3 NHC 3 NH + H 2 CCHOHCH 2 CHCHOC8H–C8H– CO + HCS + HCNH + HC 2 NCHC 2 CHOC6H–C6H– CH 2 CCHCNC3H6C3H6 CPHOC + HNCOHCOOHNH 2 CHO SiCH2OH2OHNCSH 2 CNHC5NC5N HClH2SH2SHOCO + H2C2OH2C2Ol-HC 4 H KClHNCH 2 COH 2 NCNl-HC 4 N NHHNOH 2 CNHNC 3 c-H 2 C 3 O NOMgCNH 2 CSSiH 4 H 2 CCNH NSMgNCH3O+H3O+ H 2 COH + NaClN2H+N2H+ c-SiC 3 C4H–C4H– OHN2ON2OCH 3 PNNaCN SOOCS SO + SO 2 SiNc-SiC 2 SiOCO 2 SiSNH 2 CSH3+H3+ HFH 2 D +, HD 2 + SHSiCN HDAlNC FeOSiNC O2O2 HCP CF + SiH PO >150 Molecules Detected H. S. P. Müller, F. Schlöder, J. Stutzki, and G. Winnewisser, J. Mol. Struct. 742, 215–227 (2005) H. S. P. Müller, S. Thorwirth, D. A. Roth, and G. Winnewisser, Astron. Astrophys. 370, L49–L52 (2001)

Previous Surveys of Orion KL OVRO survey 215 – 263 GHz RMS ~150 mK 800 resolved spectral features 29 molecular species IDed CSO survey 325 – 360 GHz RMS ~250 mK 717 resolved spectral features 34 molecular species IDed IRAM 30m survey , , GHz RMS ~20 mK 14,400 resolved spectral features 191 molecular species IDed

Assignment Progress Lines Observed5378 Lines Identified1094 (20.34%) Unidentified Lines4284 (79.66%) RMS30 mK Similar Surveys Completed for 4 other star forming regions and partial coverage on 7 other sources

MoleculePreviously Observed TransitionsNewly Observed Transitions HDO 21 CN 111 CO 20 DNC 10 C 17 O 10 H 2 CO 11 CH 3 CCH 24 HNCO 30 C 33 S CS 11 C 34 S 11 CH 3 CHO 445 CH 3 OH CH 3 OH 1139 HCOOCH CH 3 OCH HC 3 N 728 C 2 H 3 CN 3046 Assignment Progress

MoleculePreviously Observed TransitionsNewly Observed Transitions 13 CH 3 CN 73 CH 3 13 CN 12 CH 2 CO 12 H 2 CS 72 CH 3 CN 207 HCOOH 76 C 2 H 5 CN OCS 2 0 O 13 CS 1 1 OC 34 S 1 2 SO SO CH 3 NH CH 3 NO 012 CH 3 CH 2 OH 074 C3H6OC3H6O 070 C2H6O2C2H6O2 028 CH 2 DCN 015

Other Observatories ALMA (ESO / NAOJ / NRAO) photo by Nick Whyborn, 3 June ALMA Herschel/HIFI SOFIA O99L6VE_index_0.html

Existing Laboratory Analysis Programs Do not account for observational parameters (beam properties, telescope efficiency) Cannot input or determine physical parameters of source (temperature, column density, velocity, structure)

Existing Observational Analysis Programs Can only fit physical parameters for one molecule at a time Restricted options for spectral simulation and fitting Relies on older versions of catalogs

Program Requirements Automated line identification for multiple species Least squares analysis of spectrum for multiple species with multiple physical parameters Automated global analysis of physical conditions Ability to update laboratory spectral data for observational comparison

Assignment Methods

Automated Line Identification Automated Line Fitting Automated Boltzmann Analysis Program Goals

Acknowledgements The Widicus Weaver Group: Thomas Anderson Brandon Carroll Jay Kroll Jacob Laas Patrick Lanter Brett McGuire Susanna Widicus Weaver Caltech/CSO: Matthew Sumner Darek Lis Frank Rice Tom Phillips Geoffrey Blake CSO Local Staff