Lyα blobs like company: the discovery of a candidate 100 kpc Lyα blob near to a radio galaxy with a giant Lyα halo B3 J2330+3927 at <i>z</i> = 3.1

Matsuda, Yoshihisa; Nakamura, Yuki; Morimoto, Naotake; Smail, Ian; Breuck, C. De; Ohta, Kouji; Kodama, Tadayuki; Inoue, Akio; Hayashino, T.; Kousai, K.; Nakamura, Etsuko; Horie, Masaaki; Yamada, Tōru; Kitamura, M.; Saito, Tomoki; Taniguchi, Yoshiaki; Tanaka, Ichi; Hibon, Pascale

doi:10.1111/j.1745-3933.2009.00764.x

Cited by 46 publications

(36 citation statements)

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“…VLBA and VLA data show a one-sided jet driven by a Type II AGN (Pérez-Torres & De Breuck 2005). The galaxy environment of this Lyα blob is over-dense: a combination of broad and narrowband observations (Matsuda et al 2009) 2.2. The Instrument On UT September 18-20, 2012, we used the 6.5m MMT telescope on Mount Hopkins, Arizona, to observe B3 J2330+3927 with the SPOL CCD imaging/spectro-polarimeter in its imaging polarimetry mode (Schmidt et al 1992b).…”

Section: Introductionmentioning

confidence: 99%

“…In Section 5, we summarize our conclusions. (Matsuda et al 2009). The CO emission and H I absorption reveals a massive gas and dust reservoir associated with the radio galaxy (De Breuck et al 2003;Ivison et al 2012).…”

Section: Introductionmentioning

confidence: 99%

“…Its embedded radio galaxy is one of the 1103 radio sources from the Third Bologna Catalog (Ficarra et al 1985;Vigotti et al 1989). The associated Lyα nebula was discovered by De Breuck et al (2003) through a long-slit spectroscopy and observed in detail by Matsuda et al (2009). SPOL is a clean instrument, designed to reduce any instrument polarization by integrating over 16 different waveplate positions.…”

Section: Introductionmentioning

confidence: 99%

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MAPPING THE POLARIZATION OF THE RADIO-LOUD Lyα NEBULA B3 J2330+3927*

You

Zabludoff

Smith

et al. 2017

ApJ

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Lyα nebulae, or "Lyα blobs", are extended (up to ∼100 kpc), bright (L Lyα 10 43 erg s −1 ) clouds of Lyα emitting gas that tend to lie in overdense regions at z ∼ 2-5. The origin of the Lyα emission remains unknown, but recent theoretical work suggests that measuring the polarization might discriminate among powering mechanisms. Here we present the first narrowband, imaging polarimetry of a radio-loud Lyα nebula, B3 J2330+3927 at z = 3.09, with an embedded active galactic nucleus (AGN). The AGN lies near the blob's Lyα emission peak and its radio lobes align roughly with the blob's major axis. With the SPOL polarimeter on the 6.5m MMT telescope, we map the total (Lyα + continuum) polarization in a grid of circular apertures of radius 0.6 ′′ (4.4 kpc), detecting a significant (> 2σ) polarization fraction P % in nine apertures and achieving strong upper-limits (as low as 2%) elsewhere. P % increases from < 2% at ∼5 kpc from the blob center to 17% at ∼15-25 kpc. The detections are distributed asymmetrically, roughly along the nebula's major axis. The polarization angles θ are mostly perpendicular to this axis. Comparing the Lyα flux to that of the continuum, and conservatively assuming that the continuum is highly polarized (20-100%) and aligned with the total polarization, we place lower limits on the polarization of the Lyα emission P %,Lyα ranging from no significant polarization at ∼5 kpc from the blob center to 3-17% at 10-25 kpc. Like the total polarization, the Lyα polarization detections occur more often along the blob's major axis.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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MAPPING THE POLARIZATION OF THE RADIO-LOUD Lyα NEBULA B3 J2330+3927*

You

Zabludoff

Smith

et al. 2017

ApJ

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“…More than a few high-density regions of the Lyα emitters and star-forming galaxies at high redshift have been studied (Keel et al 1999;Steidel et al 2000Steidel et al , 2005Shimasaku et al 2003;Palunas et al 2004;Hayashino et al 2004;Matsuda et al 2004Matsuda et al , 2009Matsuda et al , 2010 Kuiper et al 2010;Yang et al 2010). Among them, the structure at z = 3.09 in the SSA22 region, specifically the area around the original selected survey area at 22 h (Cowie et al 1990), is one of the most prominent and interesting ones.…”

Section: Introductionmentioning

confidence: 99%

PANORAMIC SURVEY OF Lyα EMITTERS ATz= 3.1

Yamada

Nakamura

Matsuda

et al. 2012

The Astronomical Journal

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156

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We present the results of the extensive narrowband survey of Lyα emission-line objects at z = 3.1 in the 1.38 deg 2 area surrounding the high-density region of star-forming galaxies at z = 3.09 in the SSA22 field, as well as in the 1.04 deg 2 area of the three separated general blank fields. In total, of 2161 Lyα emitters, there are 1394 in the SSA22 fields and 767 in the general fields detected at the narrowband AB magnitude limit of 25.73, which corresponds to the line flux of ≈1.8 × 10 −17 erg s −1 cm −2 or the luminosity of ≈1.5 × 10 42 erg s −1 at z = 3.1, above the observed equivalent-width threshold, ≈190 Å. The average surface number density of the emitters at z = 3.1 in the general fields above the thresholds is 0.20 ± 0.01 arcmin −2 . The SSA22 high-density region at z = 3.09, whose peak local density is six times that of the average, is found to be the most prominent outstanding structure in the whole surveyed area and is firmly identified as a robust "protocluster." We also compared the overdensity of the 100 arcmin 2 and 700 arcmin 2 areas which contain the protocluster with the expected fluctuation of the dark matter as well as those of the model galaxies in cosmological simulations. We found that the peak height values of the overdensity are 8-10 and 3-4 times the expected standard deviations for the counts of Lyα emitters at z = 3.1 in the corresponding volume, respectively. We conclude that the structure at z = 3.09 in the SSA22 field is a very significant and rare density peak up to the scale of ≈60 Mpc.

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“…When studied in detail, these systems show complex morphologies, obscured active galactic nuclei (AGNs), and/or associated star-forming galaxies (e.g., Francis et al 1996;Ivison et al 1998;Steidel et al 2000;Palunas et al 2004;Chapman et al 2004;Matsuda et al 2004Matsuda et al , 2007Basu-Zych & Scharf 2004;Dey et al 2005;Geach et al 2007;Smith et al 2008;Prescott et al 2009;Ouchi et al 2009;Yang et al 2011). There is strong evidence that the largest Lyα nebulae are rare (Saito et al 2006;Yang et al 2009Yang et al , 2010Prescott 2009;Matsuda et al 2011) and typically reside in the most overdense regions of the universe (e.g., Palunas et al 2004;Matsuda et al 2004Matsuda et al , 2005Matsuda et al , 2009Saito et al 2006;Prescott et al 2008;Yang et al 2009). …”

Section: Introductionmentioning

confidence: 99%

RESOLVING THE GALAXIES WITHIN A GIANT Lyα NEBULA: WITNESSING THE FORMATION OF A GALAXY GROUP?

Prescott

Dey

Brodwin

et al. 2012

ApJ

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Detailed analysis of the substructure of Lyα nebulae can put important constraints on the physical mechanisms at work and the properties of galaxies forming within them. Using high-resolution Hubble Space Telescope (HST) imaging of a Lyα nebula at z ≈ 2.656, we have taken a census of the compact galaxies in the vicinity, used optical/near-infrared colors to select system members, and put constraints on the morphology of the spatially extended emission. The system is characterized by (1) a population of compact, low-luminosity (∼0.1 L * ) sources-17 primarily young, small (R e ≈ 1-2 kpc), disky galaxies including an obscured active galactic nucleus-that are all substantially offset ( 20 kpc) from the line-emitting nebula; (2) the lack of a central galaxy at or near the peak of the Lyα emission; and (3) several nearly coincident, spatially extended emission components-Lyα, He ii, and UV continuum-that are extremely smooth. These morphological findings are difficult to reconcile with theoretical models that invoke outflows, cold flows, or resonant scattering, suggesting that while all of these physical phenomena may be occurring, they are not sufficient to explain the powering and large extent of Lyα nebulae. In addition, although the compact galaxies within the system are irrelevant as power sources, the region is significantly overdense relative to the field galaxy population (by at least a factor of four). These observations provide the first estimate of the luminosity function of galaxies within an individual Lyα nebula system and suggest that large Lyα nebulae may be the seeds of galaxy groups or low-mass clusters.

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Lyα blobs like company: the discovery of a candidate 100 kpc Lyα blob near to a radio galaxy with a giant Lyα halo B3 J2330+3927 at z = 3.1

Cited by 46 publications

References 36 publications

MAPPING THE POLARIZATION OF THE RADIO-LOUD Lyα NEBULA B3 J2330+3927*

MAPPING THE POLARIZATION OF THE RADIO-LOUD Lyα NEBULA B3 J2330+3927*

PANORAMIC SURVEY OF Lyα EMITTERS ATz= 3.1

RESOLVING THE GALAXIES WITHIN A GIANT Lyα NEBULA: WITNESSING THE FORMATION OF A GALAXY GROUP?

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