Deep SAURON spectral imaging of the diffuse Lyman α halo LAB1 in SSA 22

2004/02/19 by Richard Bower, R. G. Bower, S. L. Morris +10 · 5 citations
Environmental Science · Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Emission spectrum #Galaxies: Formation, Evolution, Phenomena #Galaxy #Halo #Line (geometry) #Optics #Physics #Plant Water Relations and Carbon Dynamics #Radiative transfer #Redshift #Spectral line #astro-ph

paper · pdf · doi:10.1111/j.1365-2966.2004.07783.x

published as Mon.Not.Roy.Astron.Soc. 351 (2004) 63 · 7 pages, 5 figures. Accepted for publication in MNRAS

arxiv created 2004/02/19 · openalex publication_date 2004/06/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

We have used the SAURON panoramic integral field spectrograph to study the structure of the Lyα emission-line halo, LAB1, surrounding the submillimetre galaxy SMM J221726+0013. This emission-line halo was discovered during a narrow-band imaging survey of the z= 3.1 large-scale structure in the SSA 22 region. Our observations trace the emission halo out to almost 100 kpc from the submillimetre source and identify two distinct Lyα‘mini-haloes’ around the nearby Lyman-break galaxies. The main emission region has a broad line profile, with variations in the line profile seeming chaotic and lacking evidence for a coherent velocity structure. The data also suggest that Lyα emission is suppressed around the submillimetre source. Interpretation of the line structure needs care because Lyα may be resonantly scattered, leading to complex radiative transfer effects, and we suggest that the suppression in this region arises because of such effects. We compare the structure of the central emission-line halo with local counterparts, and find that the emission-line halo around NGC 1275 in the Perseus cluster may be a good local analogue, although the high-redshift halo is factor of ∼100 more luminous and appears to have higher velocity broadening. Around the Lyman-break galaxy C15, the emission line is narrower, and a clear shear in the emission wavelength is seen. A plausible explanation for the line profile is that the emission gas is expelled from C15 in a bipolar outflow, similar to that seen in M82.

Citations

• The Rest-Frame Optical Spectrum of MS 1512−[CLC]c[/CLC]B58
• Imaging the universe in 3D with the VLT: the next-generation field spectrometer SPIFFI
• Core condensation in heavy halos: a two-stage theory for galaxy formation and clustering
• The nature of faint submillimetre-selected galaxies
• The history of star formation in a cold dark matter universe
• A Large Structure of Galaxies at Redshiftz∼ 3 and Its Cosmological Implications
• Where Are the Baryons?
• The relationship between the optical Halpha filaments and the X-ray emission in the core of the Perseus cluster
• Deep Lyαimaging of two z = 2.04 GRB host galaxy fields
• Giant Lyα Nebulae Associated with High‐Redshift Radio Galaxies
• Radiative transfer with finite elements

Cited by

• Strategies for spectroscopy on Extremely Large Telescopes - II. Diverse-field spectroscopy
• A GIANT LYα NEBULA IN THE CORE OF AN X-RAY CLUSTER AT Z = 1.99: IMPLICATIONS FOR EARLY ENERGY INJECTION
• Large-Scale Filamentary Structure around the Protocluster at Redshift z = 3.1
• Probing Galaxy Formation with HeiiCooling Lines
• TheChandraDeep Protocluster Survey: point-source catalogues for a 400-ks observation of thez= 3.09 protocluster in SSA22
• Dissecting the Lyman α emission halo of LAB1