The Arp 240 Galaxy Merger: A Detailed Look at the Molecular Kennicutt-Schmidt Star Formation Law on Subkiloparsec Scales

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dc.catalogadorvdr
dc.contributor.authorSaravia, Alejandro
dc.contributor.authorRodas Quito, Eduardo
dc.contributor.authorBarcos Muñoz, Loreto
dc.contributor.authorEvans, Aaron
dc.contributor.authorKunneriath, Devaky
dc.contributor.authorPrivon, George
dc.contributor.authorSong, Yiqing
dc.contributor.authorYoon, Ilsang
dc.contributor.authorEmig, Kimberly L.
dc.contributor.authorSánchez Garcia, María
dc.contributor.authorLinden, Sean
dc.contributor.authorGreen, Kara Noelle
dc.contributor.authorJohnstone, Makoto
dc.contributor.authorNagarajan Swenson, Jaya
dc.contributor.authorMeza, Gabriela A.
dc.contributor.authorMomjian, Emmanuel
dc.contributor.authorArmus, Lee
dc.contributor.authorCharmandaris, Vassilis
dc.contributor.authorDíaz Santos, Tanio
dc.contributor.authorTreister, Ezequiel
dc.date.accessioned2025-03-17T13:48:24Z
dc.date.available2025-03-17T13:48:24Z
dc.date.issued2025
dc.description.abstractThe molecular Kennicutt-Schmidt Law has been key for understanding star formation (SF) in galaxies across allredshifts. However, recent subkiloparsec observations of nearby galaxies reveal deviations from the nearly unityslop e(N) obtained with disk-averaged measurements. We study SF and molecular gas (MG) distribution in theearly-stage luminous infrared galaxy merger Arp 240(NGC 5257-8). Using Very Large Array radio continuum (RC) and Atacama Large Millimeter/submillimeter Array CO(2-1)observations at 500 pc scale, with a uniformgrid analysis, we estimate SF rates and MG surface densities (Sigma(SFR) and H-2, respectively). In Arp 240,Nissublinear at 0.52 +/- 0.17. For NGC 5257 and NGC 5258,Nis 0.52 +/- 0.16 and 0.75 +/- 0.15, respectively. Weidentify two SF regimes: high surface brightness (HSB) regions in RC with N similar to 1, and low surface brightness (LSB) regions with shallow N (ranging 0.15 +/- 0.09-0.48 +/- 0.04). Median CO(2-1) linewidth and MG turbulent pressure (P-turb) are 25 km s(-1) and 9 x 10(5) K cm(-3). No significant correlation was found between Sigma(SFR) and CO(2-1) linewidth. However, Sigma(SFR) correlates with P-turb, particularly in HSB regions (rho>0.60). In contrast, SF efficiency moderately anticorrelates with P-turb in LSB regions but shows no correlation in HSB regions. Additionally, we identify regions where peaks in SF and MG are decoupled, yielding a shallow N (<= 0.28 +/- 0.18). Overall, the range of N reflects distinct physical properties and distribution of both the SF and MG, which can be masked by disk-averaged measurements.
dc.fechaingreso.objetodigital2025-03-17
dc.format.extent21 páginas
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/ad9bab
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/ad9bab
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/102654
dc.identifier.wosidWOS:001411528300001
dc.information.autorucInstituto de Astrofísica; Treister, Ezequiel; 0000-0001-7568-6412; 1031846
dc.issue.numero2
dc.language.isoen
dc.nota.accesoContenido completo
dc.pagina.final21
dc.pagina.inicio1
dc.publisherIOP Publishing Ltd
dc.revistaThe Astrophysical Journal
dc.rightsacceso abierto
dc.rights.licenseCC BY 4.0 Attribution 4.0 International
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.subject.ddc520
dc.subject.deweyAstronomíaes_ES
dc.titleThe Arp 240 Galaxy Merger: A Detailed Look at the Molecular Kennicutt-Schmidt Star Formation Law on Subkiloparsec Scales
dc.typeartículo
dc.volumen979
sipa.codpersvinculados1031846
sipa.trazabilidadWOS;2025-02-15
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