Data from the IRAM-30m Large Program `Astrochemical Surveys At IRAM' (ASAI)

Dataset for the ASAI IRAM-30m Large Program (https://www.iram-institute.org/EN/content-page-344-7-158-240-344-0.html) provided in zenodo within the framework of ACO (AstroChemical Origins): (H2020 MSCA ITN, GA:811312) The reference article is Lefloch et al. 2018, Monthly Notices of the Royal Astronomical Society, Volume 477, Issue 4, p.4792-4809 whose doi is: 10.1093/mnras/sty937 Fully reduced spectral line surveys are included for 10 young stellar objects. SOURCE SAMPLE: <br> ----------------------------------------------------------------------------------------------------------------<br> Sources alpha(2000) delta(2000) rms rms rms dnu Comment <br> (3mm) (2mm) (1.3mm) kHz<br> ----------------------------------------------------------------------------------------------------------------<br> L1544 05h04m17.2s 25d10'42.8" 2.1-7.0 - - 48.8 Evolved prestellar core<br> TMC1 04h41m41.9s 25d41'27.1" 3.0-6.3 4.2-4.2 - 48.8, 195.3 Early prestellar core<br> B1 03h33m20.8s 31d07'34.0" 2.5-10.6 4.4-8.0 4.2-4.6 195.3 First hydrostatic core<br> IRAS4A 03h29m10.4s 31d13'32.2" 2.5-3.4 5.0-6.1 4.6-3.9 195.3 Class 0: Hot corino prototype<br> L1527 04h39m53.9s 26d03'11.0" 2.1-6.7 4.2-7.1 4.6-4.1 195.3 Class 0: WCCC prototype<br> L1157mm 20h39m06.3s 68d02'15.8" 3.0-4.7 5.0-6.5 3.8-3.5 195.3 Class 0: WCCC<br> SVS13A 03h29m03.7s 31d16'03.8" 2.0-4.8 4.2-5.1 4.6-4.3 195.3 Class I: Hot corino<br> AB Aur 04h55m45.8s 30d33'33.0" 4.6-4.3 4.8-3.9 2.1-4.3 195.3 Protoplanetary disk<br> L1448-R2 03h25m40.1s 30d43'31.0" 2.8-4.9 6.0-9.7 2.9-4.9 195.3 Outflow shock spot<br> L1157-B1 20h39m10.2s 68d01'10.5" 1.1-2.9 4.6-7.2 2.1-4.2 195.3 Outflow shock spot<br> ------------------------------------------------------------------------------------------------------------------<br> i)spectral coverage, spectral resolution, and range of rms noise achieved in an element of 1 km/s for each spectral window. <br> The rms values (in TA*) are measured in the range 86-87 GHz and 113-114 GHz at 3mm, 132-133 GHz and 169-170 GHz at 2mm, <br> 220-221 and 260-261 GHz.<br> ii) No data were obtained at 2mm and 1.3mm for L1544, at 3mm and 1.3mm for TMC1. <br> iii) Complementary observations in the band 72-80 GHz have been obtained for L1544 and protostars IRAS4A, L1527, L1157mm, <br> SVS13A. The 72-80 GHz and 106-115 GHz data of L1544 will be made available in a forthcoming release<br> iv) The data of AB Aur will be made available in a forthcoming release <br> OBSERVATIONS AND SPECTRAL COVERAGE:<br> Details about the observing procedure and the calibration can be found in the article presenting ASAI: "Astrochemical evolution <br> along star formation: Overview of the IRAM Large Program ASAI" (Lefloch, Bachiller et al. 2017). L1544 80.0 - 106.0 GHz TMC1 130.0 - 164.9 GHz ; gap from 161.6 to 163.0 GHz Barnard1 80.5 - 112.2 GHz <br> 130.0 - 172.7 GHz <br> 200.5 - 276.0 GHz IRAS4A 71.7 - 79.6 GHz <br> 80.5 - 112.3 GHz <br> 125.5 - 133.3 GHz <br> 130.0 - 172.8 GHz <br> 200.5 - 276.0 GHz L1527 71.7 - 79.6 GHz <br> 80.5 - 112.3 GHz <br> 125.5 - 133.3 GHz <br> 130.0 - 172.8 GHz <br> 200.5 - 276.0 GHz L1157mm 71.7 - 79.6 GHz <br> 80.5 - 112.3 GHz <br> 125.5 - 133.3 GHz <br> 130.0 - 172.8 GHz <br> 200.5 - 276.0 GHz SVS13A 71.7 - 79.6 GHz <br> 80.5 - 116.0 GHz <br> 125.5 - 133.3 GHz <br> 130.0 - 172.8 GHz <br> 200.5 - 276.0 GHz L1448-R2 80.5 - 116.0 GHz <br> 130.0 - 173.3 GHz <br> 200.5 - 276.0 GHz <br> L1157-B1 71.7 - 79.5 GHz <br> 78.0 - 118.0 GHz; fts 390 kHz res;<br> 125.5 - 133.3 GHz <br> 128.2 - 173.7 GHz <br> 200.2 - 265.5 GHz; fts 781 kHz res;<br> 260.4 - 322.1 GHz; WILMA 2 MHz res: <br> 328.4 - 350.1 GHz; WILMA 2 MHz res; The data obtained for each source are located in the corresponding subdirectory: <br> source_f1_f2.fits : calibrated spectral band in the band f1 - f2 (in GHz) <br> source_72_80.fits : complementary data in the bands 72-80 GHz whenever observed. <br> source_125_133.fits : complementary data in the band 125.5-133.5 whenever observed. <br> UNITS:<br> The line intensity are expressed in units of antenna temperature corrected for atmospheric attenuation and the coupling with <br> the sky, TA*, by default. The interested user should to the IRAM webpage http://www.iram.es/IRAMES/mainWiki/Iram30mEfficiencies <br> to convert line intensities from antenna to main-beam temperature scale. <br> QUESTIONS and ACKNOWLEDGMENTS<br> If you have any questions about the data please contact us<br> ([e-mail], [e-mail]). We also like to hear about any<br> scientific use of the data and would appreciate acknowledgment in<br> publications or talks using the ASAI data. <br>