A Subaru Search for Lyα Blobs in and around the Protocluster Region At Redshift z = 3.1

By Y. Matsuda, T. Yamada, T. Hayashino, H. Tamura, R. Yamauchi, M. Ajiki, S. Fujita, T. Murayama, Tohru Nagao, K. Ohta and 5 more. 2004

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We report the properties of 35 robust candidate Lyα blobs (LABs), which are larger than 16 arcsec2 in isophotal area and brighter than 0.7 × 10-16 ergs s-1 cm-2, located in and around the protocluster region at redshift z = 3.1 discovered by Steidel et al. in the SSA22 field, based on wide-field (31′ × 23′) and deep narrowband (NB497; 4977 Å, FWHM 77 Å) and broadband (B, V, and R) images taken with the prime-focus camera on the Subaru Telescope. The two previously known giant LABs are the most luminous and the largest in our survey volume of 1.3 × 105 Mpc3. We reveal the internal structures of the two giant LABs and discover some bubble-like features, which suggest that intensive starburst and galactic superwind phenomena occurred in these objects in the past. The other 33 LABs have isophotal areas of ∼16–78 arcsec2 and flux of (0.7–7) × 10-16 ergs s-1 cm-2. These 35 LABs show a continuous distribution of isophotal area and emission-line flux. The distributions of average surface brightness and morphology are widespread from relatively compact high surface brightness objects to very diffuse low surface brightness ones. The physical origins of these LABs may be (1) photoionization by massive stars or active galactic nuclei, or (2) cooling radiation from gravitationally heated gas, or (3) shock heating by starburst-driven galactic superwind. One-third of the LABs are apparently not associated with ultraviolet continuum sources that are bright enough to produce Lyα emission, assuming a Salpeter initial mass function. Of these LABs 90% are located inside the high surface density region of the 283 relatively compact and strong Lyα emitters selected in our previous study. This suggests that these LABs may be phenomena related to a dense environment at high redshift.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Lyα Radiation from Collapsing Protogalaxies. I. Characteristics of the Emergent Spectrum (2005, background): “Model 2 has a steeper profile with a 1:0, and the central surface brightness is increased above the Matsuda et al. (2004) detection limit.”
SILVERRUSH. IV. Lyα luminosity functions at z = 5.7 and 6.6 studied with ∼1300 Lyα emitters on the 14–21 deg2 sky (2017, background): “…Hu 1998; Hu et al. 1998; Rhoads et al. 2000; Steidel et al. 2000; Malhotra & Rhoads 2002; Ajiki et al. 2002; Ouchi et al. 2003; Hayashino et al. 2004; Matsuda et al. 2004; Taniguchi et al. 2005; Iye et al. 2006; Kashikawa et al. 2006; Shimasaku et al. 2006; Gronwall et al. 2007; Murayama et al.…”
Evolution in the properties of Lyman-α emitters from redshifts z ~ 3 to z ~ 2 (2008, background): “Finally, Prescott et al. (2008) completed a survey ofz ∼ 2.7 LAEs around a so-called Lyα blob (e.g. Steidel et al. 2000; Matsuda et al. 2004; Dey et al. 2005; Nilsson et al. 2006).”
Systematic Identification of LAEs for Visible Exploration and Reionization Research Using Subaru HSC (SILVERRUSH). I. Program strategy and clustering properties of ∼2000 Lyα emitters at z = 6–7 over the 0.3–0.5 Gpc2 survey area (2017, background): “The bright Lyα halos extending over a few hundred kpc are known as Lyα blobs and their total Lyα luminosities are ∼1044 erg s−1 (Steidel et al. 2000; Matsuda et al. 2004; cf. Saito et al. 2006), more than an order of magnitude brighter than the diffuse Lyα halos (Momose et al. 2014, 2016).”
Extended Lyman-alpha emission from cold accretion streams (2011, background): “LABs are extremely bright (& 1043 erg s−1) and extended (& 30 kpc in diameter) Lyα nebulae (e.g. Francis et al. 1996; Keel et al. 1999; Steidel et al. 2000; Matsuda et al. 2004; Palunas et al. 2004; Nilsson et al. 2006; Smith & Jarvis 2007; Prescott et al. 2009; Yang et al. 2010; Erb et al. 2011).”
Distant radio galaxies and their environments (2008, background): “However, millimeter emission has been detected from several of these nebulae (Chapman et al 2001; Smail et al 2003; Geach et al 2005) and Matsuda et al (2004) suggest that the extended Lyα nebulae are also associated with dense environments in the early Universe.”
The realm of the galaxy protoclusters (2016, background): “However, LABs have been found also in other overdense regions not associated with radio galaxies (e.g., Francis et al., 2001; Steidel et al., 2000; Matsuda et al., 2004, 2009; Saito et al., 2006; Prescott et al., 2008, 2012; Erb et al., 2011; Hayashi et al., 2012; Cantalupo et al., 2014; Hennawi et…”
The Direct Detection of Lyman Continuum Emission from Star-forming Galaxies at z~3 (2006, background): “The narrow-band observations of Matsuda et al. (2004) indicate that Lyα emission is extended over 17 arcmin2 with a luminosity of 9.5× 1042erg s−1, and roughly centered on the R-band position of the component with detected Lyman-continuum emission.”
DIFFUSE Lyα EMITTING HALOS: A GENERIC PROPERTY OF HIGH-REDSHIFT STAR-FORMING GALAXIES (2011, background): “It was first imaged in Lyα at the same redshift by Steidel et al. (2000), who discovered two very large (> 100 kpc)“Lyα Blobs”, prompting several subsequent studies of Lyα-selected objects using deeper narrow-band data (e.g., Matsuda et al. 2004; Hayashino et al. 2004; Nestor et al. 2011).”
UBIQUITOUS GIANT Lyα NEBULAE AROUND THE BRIGHTEST QUASARS AT z ∼ 3.5 REVEALED WITH MUSE (2016, result): “…the results of other studies targeting radio-galaxies (Reuland et al. 2003; Villar-Martín et al. 2007), radio-loud quasars (Heckman et al. 1991b), Lyα blobs (Matsuda et al. 2004; Prescott et al. 2009) and other radio-quiet quasars (Bergeron et al. 1999; Christensen et al. 2006; North et al. 2012).”
The Subaru/XMM-Newton Deep Survey (SXDS). IV. Evolution of Lyα Emitters from z = 3.1 to 5.7 in the 1 deg2 Field: Luminosity Functions and AGN (2007, background): “Ly blobs are originally discovered in an overdensity region of Lymanbreak galaxies (LBGs) at z 3 (Steidel et al. 2000; Matsuda et al. 2004; see also Dey et al. 2005).”
Lyα blobs as an observational signature of cold accretion streams into galaxies (2009, methodology): “Since their discovery by Steidel et al. (2000, also see Keel et al. 1999), several tens of new LABs have been found (e.g. Matsuda et al. 2004; Dey et al. 2005; Saito et al. 2006; Smith et al. 2009).”
EVIDENCE FOR PopIII-LIKE STELLAR POPULATIONS IN THE MOST LUMINOUS Lyα EMITTERS AT THE EPOCH OF REIONIZATION: SPECTROSCOPIC CONFIRMATION (2015, background): “Both could therefore be tentatively classed as Lyα “blobs” (e.g. Steidel et al. 2000; Matsuda et al. 2004; Steidel et al. 2011).”
THE STRUCTURE AND KINEMATICS OF THE CIRCUMGALACTIC MEDIUM FROM FAR-ULTRAVIOLET SPECTRA OF z ≃ 2–3 GALAXIES (2010, background): “It is possible that the diffuse emission has already been observed in very deep Lyα images in the form of Lyα “Blobs” (Steidel et al. 2000; Matsuda et al. 2004)– the most extreme examples– or as diffuse emission evident only after stacking spatial regions surrounding normal LBGs (Hayashino et al.…”
The MUSE Hubble Ultra Deep Field Survey - VIII. Extended Lyman-α haloes around high-z star-forming galaxies (2017, background): “While some large Lyα blobs have been observed (e.g. Steidel et al. 2000; Matsuda et al. 2004, 2011), most of these studies were forced to employ stacking analyses because of sensitivity limitations.”
Lyα COOLING EMISSION FROM GALAXY FORMATION (2010, background): “Since their discovery, these blobs have become some of the most spectacular of a new class of sources that now counts several tens of members (e.g., Matsuda et al. 2004; Palunas et al. 2004; Francis et al. 2004; Dey et al. 2005; Nilsson et al. 2006; Saito et al. 2006; Smith & Jarvis 2007; Prescott…”
Large-Scale Structure of Emission-Line Galaxies at z = 3.1 (2004, methodology): “Among the 35 LABs found and discussed in Matsuda et al. (2004), 30 are included in the present extended emitter sample, while two objects are the gigantic LABs (Steidel et al. 2000) and the remaining three have smaller isophotal areas than the threshold adopted in this paper.”