J/MNRAS/514/1689 Cartwheel galaxy nebular abundances (Zaragoza-Cardiel+, 2022) ================================================================================ Nebular abundance gradient in the Cartwheel galaxy using MUSE data. Zaragoza-Cardiel J., Gomez-Gonzalez V.M.A., Mayya D., Ramos-Larios G. =2022MNRAS.514.1689Z (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Galaxies, nearby ; H II regions ; Abundances ; Optical Keywords: galaxies: star clusters - galaxies: individual - galaxies: abundances Abstract: We here present the results from a detailed analysis of nebular abundances of commonly observed ions in the collisional ring galaxy Cartwheel using the Very Large Telescope (VLT) Multi-Unit Spectroscopic Explorer (MUSE) dataset. The analysis includes 221 HII regions in the star-forming ring, in addition to 40 relatively fainter Ha-emitting regions in the spokes, disk and the inner ring. The ionic abundances of He, N, O and Fe are obtained using the direct method (DM) for 9, 20, 20, and 17 ring HII regions, respectively, where the S++ temperature-sensitive line is detected. For the rest of the regions, including all the nebulae between the inner and the outer ring, we obtained O abundances using the strong-line method (SLM). The ring regions have a median 12+log(O/H)=8.19+/-0.15, log(N/O)=-1.57+/-0.09 and log(Fe/O)=-2.24+/-0.09 using the DM. Within the range of O abundances seen in the Cartwheel, the N/O and Fe/O values decrease proportionately with increasing O, suggesting local enrichment of O without corresponding enrichment of primary N and Fe. The O abundances of the disk HII regions obtained using the SLM show a well-defined radial gradient. The mean O abundance of the ring HII regions is lower by ~0.1dex as compared to the extrapolation of the radial gradient. The observed trends suggest the preservation of the pre-collisional abundance gradient, displacement of most of the processed elements to the ring, as predicted by the recent simulation by Renaud et al. (2018MNRAS.473..585R), and post- collisional infall of metal-poor gas in the ring. Description: The main purpose of the spectral analysis is to measure accurate fluxes of emission lines suitable for nebular abundance measurements. The spectral range of MUSE includes temperature-sensitive lines of [NII] and [SIII] ions, density-sensitive lines of [SII], [ClIII] and [ArIV] ions, in addition to lines for determination of abundances of He, O, N, S, Ar, Cl, and Fe. We present the nebular abundance analysis of 221 HII regions identified in the external ring of the Cartwheel galaxy, as well as 40 regions inside the disc, using the spectroscopic data from the MUSE instrument. The complete list of lines we measured is presented in table.dat. Objects: -------------------------------------------------------- RA (2000) DE Designation(s) -------------------------------------------------------- 00 37 41.11 -33 42 58.5 Cartwheel galaxy = ESO 350-40 -------------------------------------------------------- File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table.dat 766 252 Fluxes of principal emission lines -------------------------------------------------------------------------------- Byte-by-byte Description of file: table.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 A4 --- ID Identification label (1-221, H1-H40) 6- 14 F9.7 deg RAdeg Right Ascension (J2000) 16- 25 F10.6 deg DEdeg Declination (J2000) 27- 33 F7.1 K tl ? Electron Temperature low ionization 35- 40 F6.1 K e_tl ? Electron Temperature low ionization error 42- 48 F7.1 K th ? Electron Temperature high ionization 50- 55 F6.1 K e_th ? Electron Temperature high ionization error 57- 63 F7.1 K tm ? Electron Temperature medium ionization 65- 70 F6.1 K e_tm ? Electron Temperature medium ionization error 72- 76 F5.1 e-/cm3 Ne([SII]) ? Electron density from S2 lines 78- 82 F5.1 e-/cm3 e_Ne([SII]) ? Electron density error 84- 90 E7.2 --- [FeIII/H] ? Abundance of FeIII 92- 96 E5.1 --- e_[FeIII/H] ? Abundance of FeIII error 98-105 E8.3 --- [OI/H] ? Abundance of OI 107-111 E5.1 --- e_[OI/H] ? Abundance of OI error 113-119 E7.2 --- [OII/H] ? Abundance of OII 121-125 E5.1 --- e_[OII/H] ? Abundance of OII error 127-133 E7.2 --- [OIII/H] ? Abundance of OIII 135-139 E5.1 --- e_[OIII/H] ? Abundance of OIII error 141-147 E7.2 --- [NII/H] ? Abundance of NII 149-153 E5.1 --- e_[NII/H] ? Abundance of NII error 155-161 F7.3 --- [HeI/H] ? Abundance of HeI 163-169 F7.3 --- e_[HeI/H] ? Abundance of HeI error 171-179 F9.5 --- [HeII/H] ? Abundance of HeII 181-185 E5.1 --- e_[HeII/H] ? Abundance of HeII error 187-193 E7.2 --- [Fe/H] ? Abundance of Fe 195-199 E5.1 --- e_[Fe/H] ? Abundance of Fe error 201-205 E5.1 --- [O/H] ? Abundance of O 207-211 E5.1 --- e_[O/H] ? Abundance of O error 213-219 E7.2 --- [N/H] ? Abundance of N 221-225 E5.1 --- e_[N/H] ? Abundance of N error 227-233 F7.3 --- [He/H] ? Abundance of He 235-241 F7.3 --- e_[He/H] ? Abundance of He error 243-247 F5.1 deg PA ? Position Angle 249-256 F8.3 0.1nm EWHa ? H{alpha} equivalent width 258-264 F7.3 --- AV ? Attenuation 266-272 F7.3 --- e_AV ? Attenuation error 274-278 F5.1 kpc radius ? Galactrocentric radius 280-287 F8.4 --- 12+log(O/H)s ? Oxygen abundance derived with the strong lines method 289-296 F8.4 --- e_12+log(O/H)s ? Oxygen abundance error derived with the strong lines method 298-304 F7.3 0.1nm EWHb ? H{beta} equivalent width 306-310 F5.1 --- SNRHb ? SNR of Hb flux 312-320 E9.4 mW/m2 H1r-4861A ? Attenuation-corrected flux of H1r_4861A 322-326 E5.1 mW/m2 e_H1r-4861A ? H1r-4861A error 328-333 F6.2 10-2 Fe3-4659A ? Fe3-4659A/H1r-4861A flux ratio 335-340 F6.2 10-2 e_Fe3-4659A ? Fe3-4659A/H1r-4861A flux ratio error 342-347 F6.2 10-2 He2r-4686A ? He2r-4686A/H1r-4861A flux ratio 349-354 F6.2 10-2 e_He2r-4686A ? He2r-4686A/H1r-4861A flux ratio error 356-362 F7.3 10-2 O3-4959A ? O3-4959A/H1r-4861A flux ratio 364-368 E5.1 10-2 e_O3-4959A ? O3-4959A/H1r-4861A flux ratio error 370-375 F6.2 10-2 Fe3-4986A ? Fe3-4986A/H1r-4861A flux ratio 377-382 F6.2 10-2 e_Fe3-4986A ? Fe3-4986A/H1r-4861A flux ratio error 384-390 F7.3 10-2 O3-5007A ? O3-5007A/H1r-4861AA flux ratio 392-399 F8.4 10-2 e_O3-5007A ? O3-5007A/H1r-4861A flux ratio error 401-407 F7.3 10-2 He1r-5876A ? He1r-5876A/H1r-4861A flux ratio 409-415 F7.3 10-2 e_He1r-5876A ? He1r-5876A/H1r-4861A flux ratio error 417-423 F7.3 10-2 O1-6300A ? O1-6300A/H1r-4861A flux ratio 425-431 F7.3 10-2 e_O1-6300A ? O1-6300A/H1r-4861A flux ratio error 433-439 F7.3 10-2 S3-6312A ? S3-6312A/H1r-4861A flux ratio 441-447 F7.3 10-2 e_S3-6312A ? S3-6312A/H1r-4861A flux ratio error 449-454 F6.2 10-2 O1-6364A ? O1-6364A/H1r-4861A flux ratio 456-461 F6.2 10-2 e_O1-6364A ? O1-6364A/H1r-4861A flux ratio error 463-469 F7.3 10-2 N2-6548A ? N2-6548A/H1r-4861A flux ratio 471-478 F8.4 10-2 e_N2-6548A ? N2-6548A/H1r-4861A flux ratio error 480-485 F6.2 10-2 H1r-6563A ? H1r-6563A/H1r-4861A flux ratio 487-494 F8.4 10-2 e_H1r-6563A ? H1r-6563A/H1r-4861A flux ratio error 496-502 F7.3 10-2 N2-6584A ? N2-6584A/H1r-4861A flux ratio 504-511 F8.4 10-2 e_N2-6584A ? N2-6584A/H1r-4861A flux ratio error 513-519 F7.3 10-2 He1r-6678A ? He1r-6678A/H1r-4861A flux ratio 521-527 F7.3 10-2 e_He1r-6678A ? He1r-6678A/H1r-4861A flux ratio error 529-535 F7.3 10-2 S2-6716A ? S2-6716A/H1r-4861A flux ratio 537-541 E5.1 10-2 e_S2-6716A ? S2-6716A/H1r-4861A flux ratio error 543-549 F7.3 10-2 S2-6731A ? S2-6731A/H1r-4861A flux ratio 551-558 F8.4 10-2 e_S2-6731A ? S2-6731A/H1r-4861A flux ratio error 560-565 F6.2 10-2 O2-7319A ? O2-7319A/H1r-4861A flux ratio 567-572 F6.2 10-2 e_O2-7319A ? O2-7319A/H1r-4861A flux ratio error 574-579 F6.2 10-2 O2-7330A ? O2-7330A/H1r-4861A flux ratio 581-586 F6.2 10-2 e_O2-7330A ? O2-7330A/H1r-4861A flux ratio error 588-593 F6.2 10-2 Ar3-7751A ? Ar3-7751A/H1r-4861A flux ratio 595-600 F6.2 10-2 e_Ar3-7751A ? Ar3-7751A/H1r-4861A flux ratio error 602-607 F6.2 10-2 O1-8446A ? O1-8446A/H1r-4861A flux ratio 609-614 F6.2 10-2 e_O1-8446A ? O1-8446A/H1r-4861A flux ratio error 616-622 F7.3 10-2 S3-9069A ? S3-9069A/H1r-4861A flux ratio 624-630 F7.3 10-2 e_S3-9069A ? S3-9069A/H1r-4861A flux ratio error 632-638 F7.3 10-2 He1r-7065A ? He1r-7065A/H1r-4861A flux ratio 640-646 F7.3 10-2 e_He1r-7065A ? He1r-7065A/H1r-4861A flux ratio error 648-653 F6.2 10-2 Ar4-4711A ? Ar4-4711A/H1r-4861A flux ratio 655-660 F6.2 10-2 e_Ar4-4711A ? Ar4-4711A/H1r-4861A flux ratio error 662-667 F6.2 10-2 Ar4-4740A ? Ar4-4740A/H1r-4861A flux ratio 669-674 F6.2 10-2 e_Ar4-4740A ? Ar4-4740A/H1r-4861A flux ratio error 676-681 F6.2 10-2 He1r-4922A ? He1r-4922A/H1r-4861A flux ratio 683-688 F6.2 10-2 e_He1r-4922A ? He1r-4922A/H1r-4861A flux ratio error 690-694 F5.1 10-2 Fe3-5270A ? Fe3-5270A/H1r-4861A flux ratio 696-700 F5.1 10-2 e_Fe3-5270A ? Fe3-5270A/H1r-4861A flux ratio error 702-706 F5.1 10-2 He1r-7281A ? He1r-7281A/H1r-4861A flux ratio 708-712 F5.1 10-2 e_He1r-7281A ? He1r-7281A/H1r-4861A flux ratio error 714-720 F7.3 10-2 He1r-5016A ? He1r-5016A/H1r-4861A flux ratio 722-728 F7.3 10-2 e_He1r-5016A ? He1r-5016A/H1r-4861A flux ratio error 730-735 F6.2 10-2 N2-5755A ? N2-5755A/H1r-4861A flux ratio 737-742 F6.2 10-2 e_N2-5755A ? N2-5755A/H1r-4861A flux ratio error 744-748 F5.1 10-2 Fe3-4701A ? Fe3-4701A/H1r-4861A flux ratio 750-754 F5.1 10-2 e_Fe3-4701A ? Fe3-4701A/H1r-4861A flux ratio error 756-760 F5.1 10-2 He1r-5048A ? He1r-5048A/H1r-4861A flux ratio 762-766 F5.1 10-2 e_He1r-5048A ? He1r-5048A/H1r-4861A flux ratio error -------------------------------------------------------------------------------- Acknowledgements: Javier Zaragoza-Cardiel, javier.zaragoza(at)inaoep.mx ================================================================================ (End) Patricia Vannier [CDS] 18-Aug-2022