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Intergalactic Medium Emission Observations with the Cosmic Web Imager. II. Discovery of Extended, Kinematically-Linked Emission around SSA22 Lyα Blob 2

Martin, D. Christopher and Chang, Daphne and Matuszewski, Matt and Morrissey, Patrick and Rahman, Shahin and Moore, Anna and Steidel, Charles C. and Matsuda, Yuichi (2014) Intergalactic Medium Emission Observations with the Cosmic Web Imager. II. Discovery of Extended, Kinematically-Linked Emission around SSA22 Lyα Blob 2. Astrophysical Journal, 786 (2). Art. No. 107. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20140303-145821259

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Abstract

The intergalactic medium (IGM) is the dominant reservoir of baryons, delineates the large scale structure of the universe at low to moderate overdensities, and provides gas from which galaxies form and evolve. Simulations of a Cold Dark Matter (CDM) dominated universe predict that the IGM is distributed in a cosmic web of filaments, and that galaxies should form along and at the intersections of these filaments (Bond, Kofman, & Pogosyan 1994; Miralda-Escude et al. 1996). While observations of QSO absorption lines and the large-scale distribution of galaxies have confirmed the CDM paradigm, the cosmic web of IGM has never been confirmed by direct imaging. Here we report our observation of the Lyα blob-2 (LAB2) in SSA22, with the Cosmic Web Imager. This is an integral field spectrograph optimized for low surface brightness, extended emission. With 22 hours of total on- and off-source exposure, CWI has revealed that LAB2 has extended Lyα emission which is organized into azimuthal zones consistent with filaments. We perform numerous tests with simulations and the data to secure the robustness of this result, which relies on data with modest signal-to-noise ratio. We have developed a smoothing algorithm that permits visualization of data cube slices along image or spectral-image planes. With both raw and smoothed data cubes we demonstrate that the filaments are kinematically associated with LAB2 and display double-peaked profiles characteristic of optically thick Lyα emission. The flux is 10-20 times brighter than expected for the average emission from the IGM but is consistent with boosted fluorescence from a buried QSO or gravitation cooling radiation. Using simple emission models we infer a baryon mass in the filaments of at least 1−4 × 10^(11)M_☉, and the dark halo mass is at least 2 × 10^(12)M_☉. The spatial-kinematic morphology is more consistent with inflow from the cosmic web than outflow from LAB2, although an outflow feature maybe present at one azimuth. LAB2 and the surrounding gas have significant and coaligned angular momentum, strengthening the case for their association.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1402.4809arXivDiscussion Paper
http://dx.doi.org/10.1088/0004-637X/786/2/107DOIArticle
http://iopscience.iop.org/0004-637X/786/2/107/articlePublisherArticle
Additional Information:© 2014. The American Astronomical Society. Received 2013 May 24; accepted 2013 October 31; published 2014 April 24. We thank Tom Tombrello and Shri Kulkarni for their support of CWI. We thank Marty Crabill, Steve Kaye and the staff of the Palomar Observatory for their constant support. Nicole Ligner participated in the observations. We are deeply grateful to Dean Joe Shepard, to the Caltech Counselling Office, and to the family of Daphne Chang for their strength and support. The anonymous referee provided excellent suggestions that significantly improved the paper. This work was supported by the National Science Foundation and the California Institute of Technology.
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Subject Keywords:galaxies: evolution – galaxies: formation – galaxies: high-redshift – intergalactic medium – techniques: imaging spectroscopy
Record Number:CaltechAUTHORS:20140303-145821259
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140303-145821259
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:44105
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:03 Mar 2014 23:34
Last Modified:18 Jun 2014 19:05

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