“HI巡天”的版本间差异

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* Catalog [https://arxiv.org/abs/2011.02588]
* Catalog [https://arxiv.org/abs/2011.02588]
* data webpage [http://egg.astro.cornell.edu/alfalfa/data/index.php]
* data webpage [http://egg.astro.cornell.edu/alfalfa/data/index.php]
*发现了一下Ha dots [[https://arxiv.org/abs/2112.02135]


==Galaxy==
==Galaxy==
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*Nançay Interstellar Baryons Legacy Extragalactic Survey (NanCay Radio Telescop 100m)
*Nançay Interstellar Baryons Legacy Extragalactic Survey (NanCay Radio Telescop 100m)
#Must have both SDSS magnitudes and optical spectrum;
#Must have both SDSS magnitudes and optical spectrum;
#Must lie within the local volume (900<cz<12,000 km s−1);
#Must lie within the [[local volume]] (900<cz<12,000 km s−1);
#Uniform sampling of each 0.5 magnitude wide bin in absolute z-band magnitude, Mz;
#Uniform sampling of each 0.5 magnitude wide bin in absolute z-band magnitude, Mz;
#Preferentially observe nearby objects;
#Preferentially observe nearby objects;

2021年12月12日 (日) 14:00的最新版本

Blind Survey

HIPASS

  • The HI Parkes All-Sky Survey (HIPASS) covered 30000 deg2 and produced a final catalog of around 5000 HI detections with a median redshift of 2800 km/s.

ALFALFA

  • Arecibo Legacy Fast ALFA Survey (ALFALFA) will map 7000 deg2 and is expected to detect more than 25,000 extragalactic HI line sources out to redshifts of 18,000 km/s.
  • the spatial resolution of the grid to 4.3'x3.8'
  • spectral velocity resolution is 11 km/s after smoothing is applied,
  • Catalog [1]
  • data webpage [2]
  • 发现了一下Ha dots [[3]

Galaxy

AGES

  • Arecibo Galaxy Environment Survey (AGES), will cover a total area of 200 deg2 (divided into 13 predesignated regions to sample different environments) to greater depth

THINGS

  • The H I Nearby Galaxy Survey (THINGS)," a high spectral (≤5.2 km s–1) and spatial (~6) resolution survey of H I emission in 34 nearby galaxies obtained using the NRAO Very Large Array (VLA).
  • public data [4]

NIBLES

  • Nançay Interstellar Baryons Legacy Extragalactic Survey (NanCay Radio Telescop 100m)
  1. Must have both SDSS magnitudes and optical spectrum;
  2. Must lie within the local volume (900<cz<12,000 km s−1);
  3. Uniform sampling of each 0.5 magnitude wide bin in absolute z-band magnitude, Mz;
  4. Preferentially observe nearby objects;
  5. No a priori selection on color.
  • 这种on source的观测比ALFALFA这种盲测的好更高信噪比,但是还是有一些星系用了Arecibo做了follow up的定点观测,灵敏度更高,可以到mJy以下,(可以探测Lr < 10^8.5的蓝星系)。参见[5]