First detection of [CII]158 μm at high redshift : vigorous star formation in the early universe

By R. Maiolino, P. Cox, P. Caselli, A. Beelen, F. Bertoldi, C. Carilli, M. Kaufman, K. Menten, Tohru Nagao, A. Omont and 3 more. 2005

201 citations recorded by the source corpus.

We report the detection of the $^2\rm P_{3/2} \rightarrow {^2P_{1/2}}$ fine-structure line of $\rm C^+$ at 157.74 $\rm \mu m$ in SDSS J114816.64+525150.3 (hereafter J1148+5251), the most distant known quasar, at $z=6.42$, using the IRAM 30-m telescope. This is the first detection of the [Cii] line at high redshift, and also the first detection in a Hyperluminous Infrared Galaxy ($L_{\rm FIR} > 10^{13} \, L_\odot$). The [Cii] line is detected at a significance level of 8 σ and has a luminosity of $ 4.4\times 10^9 \,L_\odot$. The $L_{\rm [CII]}/L_{\rm FIR}$ ratio is $\rm 2\times 10^{-4}$, about an order of magnitude smaller than observed in local normal galaxies and similar to the ratio observed in local Ultraluminous Infrared Galaxies. The [Cii] line luminosity indicates that the host galaxy of this quasar is undergoing an intense burst of star formation with an estimated rate of ≈ $ 3000 \, M_\odot \, \rm yr^{-1}$. The detection of $\rm C^+$ in SDSS J1148+5251 suggests a significant enrichment of metals at $z\sim 6$ (age of the universe ~870 Myr), although the data are consistent with a reduced carbon to oxygen ratio as expected from chemical evolutionary models of the early phases of galaxy formation.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d55ac398eb109e929b998bbf8704ad137438a4ec

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Stellar sources of dust in the high-redshift Universe (2009, background): “In fact, the detection of metal lines such as Fe (Barth et al. 2003), CII (Maiolino et al. 2005), and OI (in absorption, Becker et al. 2006) indicates that the ISM of the QSO host was significantly enriched by heavy elements.”
Terahertz Spectroscopy for Astronomy: From Comets to Cosmology (2011, methodology): “C and CO emission was detected from a hyper-luminous galaxy at a redshift of 6.42 [68]–[ 70 ], the first detection of C at truly cosmological distances and in a galaxy with an infrared luminosity M . Further detections and imaging of CO and C in high redshift objects will be a key focus of the Ataca”
A 158 μm [C ii] LINE SURVEY OF GALAXIES AT z ∼ 1–2: AN INDICATOR OF STAR FORMATION IN THE EARLY UNIVERSE (2010, background): “To date, three detections of [C ii] from extreme luminosity (LFIR >1013 L ) systems at very high redshift have been reported (SDSS F1148, Maiolino et al. 2005; BR 1202–0725, Iono et al. 2006a; and BRI 0952–0115, Maiolino et al. 2009) together with additional two systems with scientifically…”
SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9 (2016, unknown): “…be studied in the optical/infrared (e.g., Kashikawa et al. 2007; Goto et al. 2009, 2012; Willott et al. 2011) or at sub-mm/radio wavelengths (e.g., Maiolino et al. 2005; Wang et al. 2007; Venemans et al. 2012, 2016; Wang et al. 2013; Willott et al. 2013, 2015), giving a unique probe of galaxies…”
350 μm Dust Emission from High-Redshift Quasars (2006, background): “Amassive reservoir of densemolecular gas ( 2 ; 1010 M ) is implied by the observed CO emission (Walter et al. 2003; Bertoldi et al. 2003b) and the recent detection of the [C ii] emission line (Maiolino et al. 2005).”
The assembly of ‘normal’ galaxies at z ∼ 7 probed by ALMA (2015, background): “At z>4 mm/submm observations are even more effective since the luminous [CII]158µm far-infrared fine structure line is redshifted into the primary bands of atmospheric transmission, at frequencies ν < 350GHz (Maiolino et al. 2005, 2009; Walter et al. 2009; De Breuck et al. 2011).”
An ALMA [C ii] Survey of 27 Quasars at z > 5.94 (2018, background): “We therefore included this object in the sample. from Maiolino et al. (2005) and Walter et al. (2009); one quasar from Bañados et al. (2015); five quasars from Venemans et al. (2012, 2016, 2017a, 2017c); five from Willott et al. (2013, 2015, 2017);14 four quasars from Wang et al. (2013, 2016); and…”
Direct Cosmological Simulations of the Growth of Black Holes and Galaxies (2007, background): “CO observations indicate a relatively small stellar spheroid; however, the existence of CO, iron, and carbon emission indicates a heavily enriched ISM and vigorous star formation (Maiolino et al. 2005).”
Four Quasars above Redshift 6 Discovered by the Canada-France High-z Quasar Survey (2007, background): “J1148+5251 is also the first high-z source where [CII ] line emission was detected (Maiolino et al. 2005).”
Very extended cold gas, star formation and outflows in the halo of a bright QSO at z>6 (2014, background): “At the redshift of the source (z = 6.4189, Maiolino et al. 2005), the [C ii] 158 μm transition is redshifted into the 1 mm band, at an observed frequency of 256.175 GHz.”
Star Formation in the Hosts of High-z QSOs: Evidence from Spitzer PAH Detections (2008, background): “Finally, the [CII] 157µm fine structure line was detected in a few high-z quasars (Maiolino et al. 2005; Iono et al. 2006) at a ratio to the rest frame far-infrared emission similar to the ratio in local ULIRGs, consistent with massive star formation.”
Black Hole Masses and Enrichment of z ~ 6 SDSS Quasars (2007, background): “The detection of [C II 158µm] emission in this QSO by Maiolino et al. (2005) shows that its host is undergoing an intense burst of star formation.”
ALMA IMAGING OF GAS AND DUST IN A GALAXY PROTOCLUSTER AT REDSHIFT 5.3: [C ii] EMISSION IN “TYPICAL” GALAXIES AND DUSTY STARBURSTS ≈1 BILLION YEARS AFTER THE BIG BANG (2014, background): “…of the ISM out to the most distant galaxies, but it was only detected in some of the most luminous quasars and starburst galaxies in the past (e.g., Maiolino et al. 2005, 2009; Walter et al. 2009; Stacey et al. 2010; Wagg et al. 2010; Valtchanov et al. 2011; Riechers et al. 2013; Wang et al. 11…”
STAR FORMATION AND GAS KINEMATICS OF QUASAR HOST GALAXIES AT z ∼ 6: NEW INSIGHTS FROM ALMA (2013, background): “…of 1.5× the FWHM major axis from the [C ii] intensity map (i.e., full width at 20% of the peak intensity for a Gaussian profile). detections in this work, J1148+5251 (Maiolino et al. 2005), CFHQS J0210−0456 at z = 6.43 (Willott et al. 2013), and ULAS J1120+0640 at z = 7.08 (Venemans et al. 2012).”
AN INTENSELY STAR-FORMING GALAXY AT z ∼ 7 WITH LOW DUST AND METAL CONTENT REVEALED BY DEEP ALMA AND HST OBSERVATIONS (2013, background): “Although a few QSOs have been observed at sub-mm wavelengths to z = 6.4 − 7.1 (Maiolino et al. 2005; Iono et al. 2006; Walter et al. 2009; Venemans et al. 2012; Willott et al. 2013; Wang et al. 2013), the presence of a powerful AGN undoubtedly complicates any understanding of the physical…”
Dusty Star Forming Galaxies at High Redshift (2014, background): “Luminous quasar host galaxies (e.g. Maiolino et al., 2005; Iono et al., 2006; Maiolino et al., 2009;Walter et al., 2009;Wagg et al., 2010; Stacey et al., 2010; Gallerani et al., 2012; Carniani et al., 2013), SMGs (e.g. Ivison et al., 2010d; Stacey et al., 2010; Cox et al., 2011; De Breuck et al.,…”
Evidence of strong quasar feedback in the early Universe (2012, background): “The spectrum shows a clear narrow [CII]158µm emission line, which was already detected by previous observations (Maiolino et al. 2005; Walter et al. 2009).”
GAS AND DUST IN A SUBMILLIMETER GALAXY AT z = 4.24 FROM THE HERSCHEL ATLAS (2011, unknown): “…value of LC ii for ID 141 is therefore comparable to that of other high-redshift sources, such as: SDSS J1148+5251 (z = 6.42) with (4.4 ± 0.5) × 109 L (Maiolino et al. 2005; Walter et al. 2009), BR 0952−0115 (z = 4.43) with (4.6 ± 0.7) × 109 L (Maiolino et al. 2009), BRI 1335−0417 (z = 4.40) with…”