TY - JOUR

T1 - Starburst to Quiescent from HST/ALMA

T2 - Stars and Dust Unveil Minor Mergers in Submillimeter Galaxies at z ∼ 4.5

AU - Gómez-Guijarro, C.

AU - Toft, S.

AU - Karim, A.

AU - Magnelli, B.

AU - Magdis, G. E.

AU - Jiménez-Andrade, E. F.

AU - Capak, P. L.

AU - Fraternali, F.

AU - Fujimoto, S.

AU - Riechers, D. A.

AU - Schinnerer, E.

AU - Smolčić, V.

AU - Aravena, M.

AU - Bertoldi, F.

AU - Cortzen, I.

AU - Hasinger, G.

AU - Hu, E. M.

AU - Jones, G. C.

AU - Koekemoer, A. M.

AU - Lee, N.

AU - McCracken, H. J.

AU - Michałowski, M. J.

AU - Navarrete, F.

AU - Pović, M.

AU - Puglisi, A.

AU - Romano-Díaz, E.

AU - Sheth, K.

AU - Silverman, J. D.

AU - Staguhn, J.

AU - Steinhardt, C. L.

AU - Stockmann, M.

AU - Tanaka, M.

AU - Valentino, F.

AU - van Kampen, E.

AU - Zirm, A.

PY - 2018/4/1

Y1 - 2018/4/1

N2 - Dust-enshrouded, starbursting, submillimeter galaxies (SMGs) at z ≥ 3 have been proposed as progenitors of z ≥ 2 compact quiescent galaxies (cQGs). To test this connection, we present a detailed spatially resolved study of the stars, dust, and stellar mass in a sample of six submillimeter-bright starburst galaxies at z ∼ 4.5. The stellar UV emission probed by HST is extended and irregular and shows evidence of multiple components. Informed by HST, we deblend Spitzer/IRAC data at rest-frame optical, finding that the systems are undergoing minor mergers with a typical stellar mass ratio of 1:6.5. The FIR dust continuum emission traced by ALMA locates the bulk of star formation in extremely compact regions (median r e = 0.70 ± 0.29 kpc), and it is in all cases associated with the most massive component of the mergers (median {log}({M}* /{M}ȯ )=10.49+/- 0.32). We compare spatially resolved UV slope (β) maps with the FIR dust continuum to study the infrared excess (IRX = L IR/L UV)–β relation. The SMGs display systematically higher IRX values than expected from the nominal trend, demonstrating that the FIR and UV emissions are spatially disconnected. Finally, we show that the SMGs fall on the mass–size plane at smaller stellar masses and sizes than the cQGs at z = 2. Taking into account the expected evolution in stellar mass and size between z = 4.5 and z = 2 due to the ongoing starburst and mergers with minor companions, this is in agreement with a direct evolutionary connection between the two populations.

AB - Dust-enshrouded, starbursting, submillimeter galaxies (SMGs) at z ≥ 3 have been proposed as progenitors of z ≥ 2 compact quiescent galaxies (cQGs). To test this connection, we present a detailed spatially resolved study of the stars, dust, and stellar mass in a sample of six submillimeter-bright starburst galaxies at z ∼ 4.5. The stellar UV emission probed by HST is extended and irregular and shows evidence of multiple components. Informed by HST, we deblend Spitzer/IRAC data at rest-frame optical, finding that the systems are undergoing minor mergers with a typical stellar mass ratio of 1:6.5. The FIR dust continuum emission traced by ALMA locates the bulk of star formation in extremely compact regions (median r e = 0.70 ± 0.29 kpc), and it is in all cases associated with the most massive component of the mergers (median {log}({M}* /{M}ȯ )=10.49+/- 0.32). We compare spatially resolved UV slope (β) maps with the FIR dust continuum to study the infrared excess (IRX = L IR/L UV)–β relation. The SMGs display systematically higher IRX values than expected from the nominal trend, demonstrating that the FIR and UV emissions are spatially disconnected. Finally, we show that the SMGs fall on the mass–size plane at smaller stellar masses and sizes than the cQGs at z = 2. Taking into account the expected evolution in stellar mass and size between z = 4.5 and z = 2 due to the ongoing starburst and mergers with minor companions, this is in agreement with a direct evolutionary connection between the two populations.

KW - galaxies: evolution

KW - galaxies: formation

KW - galaxies: high-redshift

KW - galaxies: interactions

KW - galaxies: ISM

KW - galaxies: starburst

U2 - 10.3847/1538-4357/aab206

DO - 10.3847/1538-4357/aab206

M3 - Journal article

VL - 856

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 121

ER -