Deep Lens Survey

The Deep Lens Survey (DLS, short for "Deep Gravitational Lensing Survey") is an ultra-deep multi-band optical survey of seven 4 square degree fields. Mosaic CCD imagers at the National Optical Astronomy Observatory's Blanco (Cerro Tololo) and Mayall telescopes (Kitt Peak) are being used. The deep fields took five years to complete (2001–2006), in four bands: B, V, R, and z', to 29/29/29/28 mag per square arcsecond surface brightness. Optical transient events (including moving objects such as minor planets and comets) and supernova candidates are released in real time.

Deep Lens Survey
Survey typeastronomical survey 
Targetgravitational lens 
Minor planets discovered: 79 [1]
see § List of discovered minor planets

Survey

The main goal of the survey is to produce unbiased maps of the large-scale structure of the mass distribution beyond the local universe, via very deep multicolor imaging of seven 2-degree fields and colour-redshifts. The shear of distant galaxies induced by the mass of foreground structures will be measured. These weak-lensing observations are sensitive to all forms of clumped mass and will yield unbiased mass maps with resolution of one arcmin in the plane of the sky (about 120 kpc/h at z = 0.2), in multiple redshift ranges. These maps will measure for the first time the change in large scale structure from z = 1 to the present epoch, and test the current theories of structure formation, which predict that mass in the low-redshift universe has a particular filamentary/sheetlike structure. These observations will directly constrain the clustering properties of matter, and, when compared with the results from microwave background anisotropy missions, will test the basic theory of structure formation via gravitational instability.

While this is the main goal of the survey, a wide-field imaging survey has a myriad of other uses. In addition, the group is acquiring the data in a way which makes it possible to detect variable objects on scales of hours to months, by spreading observations of individual subfields over 4 runs over two years.

Discoveries

List of discovered minor planets
(46060) 2001 DL8826 February 2001list
(89886) 2002 CT23014 February 2002list
(104314) 2000 EC2035 March 2000list
(107558) 2001 DK8523 February 2001list
(107868) 2001 FT8526 March 2001list
(114722) 2003 GN333 April 2003list
(143352) 2003 AB857 January 2003list
(144688) 2004 FG14529 March 2004list
(147428) 2003 GM541 April 2003list
(148990) 2001 YX9217 December 2001list
(154544) 2003 GP334 April 2003list
(156423) 2002 AD9212 January 2002list
(159758) 2003 FZ12231 March 2003list
(160842) 2000 YE14221 December 2000list
(189839) 2003 AQ834 January 2003list
(193671) 2001 DV8423 February 2001list
(196401) 2003 GM333 April 2003list
(205413) 2001 FX8526 March 2001list
(208544) 2002 AE9212 January 2002list
(216501) 2000 EP2035 March 2000list
(220530) 2004 FT1826 March 2004list
(223271) 2003 GY321 April 2003list
(223272) 2003 GC331 April 2003list
(226345) 2003 FM12231 March 2003list
(231056) 2005 JG633 May 2005list
(231914) 2000 YT14019 December 2000list
(242393) 2004 FO1826 March 2004list
(242599) 2005 JG452 May 2005list
(244218) 2002 AA9314 January 2002list
(245421) 2005 JW634 May 2005list
(245431) 2005 JX1086 May 2005list
(252143) 2000 YK14120 December 2000list
(257954) 2000 YY14120 December 2000list
(264468) 2001 FY8526 March 2001list
(267852) 2003 UJ28330 October 2003list
(270019) 2001 FA8626 March 2001list
(270473) 2002 DV417 February 2002list
(275636) 2000 EJ2035 March 2000list
(283757) 2003 EU618 March 2003list
(285797) 2000 WN19324 November 2000list
(285835) 2001 DW8323 February 2001list
(287594) 2003 FK12231 March 2003list
(297152) 2010 UQ5614 February 2002list
(301831) 2011 QH145 March 2000list
(302421) 2002 CU23014 February 2002list
(302806) 2003 AH834 January 2003list
(302864) 2003 GJ541 April 2003list
(306179) 2010 WA552 April 2003list
(306339) 2011 SQ1295 January 2003list
(306581) 2000 ED2046 March 2000list
(317662) 2003 FY12231 March 2003list
(318601) 2005 JX453 May 2005list
(321876) 2010 SG723 February 2001list
(337289) 2000 WL19425 November 2000list
(338450) 2003 EG559 March 2003list
(348151) 2004 FS1826 March 2004list
(354650) 2005 JR453 May 2005list
(357315) 2003 FL12231 March 2003list
(360809) 2005 JH633 May 2005list
(365944) 2012 AZ169 March 2003list
(368103) 2013 EN3 May 2005list
(370195) 2002 CU23115 February 2002list
(370686) 2004 FS12326 March 2004list
(385437) 2003 GH551 April 2003list
(393559) 2003 GO333 April 2003list
(397214) 2006 GU372 April 2006list
(415789) 2000 WO19324 November 2000list
(416827) 2005 JU453 May 2005list
(416834) 2005 JY1086 May 2005list
(416835) 2005 JA1096 May 2005list
(427831) 2005 JQ1084 May 2005list
(434011) 2000 YU14019 December 2000list
(455743) 2005 JV453 May 2005list
(461503) 2003 FJ12231 March 2003list
(461672) 2005 JM226 May 2005list
(464869) 2005 JL224 May 2005list
(464881) 2005 JF1775 May 2005list
(468500) 2005 JR1086 May 2005list
(481053) 2005 JP453 May 2005list

Galaxy clusters
Significant discoveries
Cluster Date Notes Names Refs
DLSCL J0916.2+2951 2012 This is a dissociative galaxy cluster merger with a large separation between the baryonic and dark matter components. Musket Ball Cluster [2][3]

References
  1. "Minor Planet Discoverers (by number)". Minor Planet Center. 12 January 2017. Retrieved 2 February 2017.
  2. Dawson, William A.; Wittman, David; Jee, M. James; Gee, Perry; Hughes, John P.; Tyson, J. Anthony; et al. (19 October 2011). "Discovery of a Dissociative Galaxy Cluster Merger with Large Physical Separation". The Astrophysical Journal Letters (published March 2012). 747 (2): 6. arXiv:1110.4391. Bibcode:2012ApJ...747L..42D. doi:10.1088/2041-8205/747/2/L42. L42.
  3. Chandra X-Ray Observatory (12 April 2012). "DLSCL J0916.2+2951: Discovery of the Musket Ball Cluster". Harvard University.
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