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Deep Lens Survey
Alternative names	"Deep Gravitational Lensing Survey"
	[edit on Wikidata]

Minor planets discovered: 79 ^[1]
see § List of discovered minor planets

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.

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 DL₈₈	26 February 2001	list
(89886) 2002 CT₂₃₀	14 February 2002	list
(104314) 2000 EC₂₀₃	5 March 2000	list
(107558) 2001 DK₈₅	23 February 2001	list
(107868) 2001 FT₈₅	26 March 2001	list
(114722) 2003 GN₃₃	3 April 2003	list
(143352) 2003 AB₈₅	7 January 2003	list
(144688) 2004 FG₁₄₅	29 March 2004	list
(147428) 2003 GM₅₄	1 April 2003	list
(148990) 2001 YX₉₂	17 December 2001	list
(154544) 2003 GP₃₃	4 April 2003	list
(156423) 2002 AD₉₂	12 January 2002	list
(159758) 2003 FZ₁₂₂	31 March 2003	list
(160842) 2000 YE₁₄₂	21 December 2000	list
(189839) 2003 AQ₈₃	4 January 2003	list
(193671) 2001 DV₈₄	23 February 2001	list
(196401) 2003 GM₃₃	3 April 2003	list
(205413) 2001 FX₈₅	26 March 2001	list
(208544) 2002 AE₉₂	12 January 2002	list
(216501) 2000 EP₂₀₃	5 March 2000	list
(220530) 2004 FT₁₈	26 March 2004	list
(223271) 2003 GY₃₂	1 April 2003	list
(223272) 2003 GC₃₃	1 April 2003	list
(226345) 2003 FM₁₂₂	31 March 2003	list
(231056) 2005 JG₆₃	3 May 2005	list

(231914) 2000 YT₁₄₀	19 December 2000	list
(242393) 2004 FO₁₈	26 March 2004	list
(242599) 2005 JG₄₅	2 May 2005	list
(244218) 2002 AA₉₃	14 January 2002	list
(245421) 2005 JW₆₃	4 May 2005	list
(245431) 2005 JX₁₀₈	6 May 2005	list
(252143) 2000 YK₁₄₁	20 December 2000	list
(257954) 2000 YY₁₄₁	20 December 2000	list
(264468) 2001 FY₈₅	26 March 2001	list
(267852) 2003 UJ₂₈₃	30 October 2003	list
(270019) 2001 FA₈₆	26 March 2001	list
(270473) 2002 DV₄	17 February 2002	list
(275636) 2000 EJ₂₀₃	5 March 2000	list
(283757) 2003 EU₆₁	8 March 2003	list
(285797) 2000 WN₁₉₃	24 November 2000	list
(285835) 2001 DW₈₃	23 February 2001	list
(287594) 2003 FK₁₂₂	31 March 2003	list
(297152) 2010 UQ₅₆	14 February 2002	list
(301831) 2011 QH₁₄	5 March 2000	list
(302421) 2002 CU₂₃₀	14 February 2002	list
(302806) 2003 AH₈₃	4 January 2003	list
(302864) 2003 GJ₅₄	1 April 2003	list
(306179) 2010 WA₅₅	2 April 2003	list
(306339) 2011 SQ₁₂₉	5 January 2003	list
(306581) 2000 ED₂₀₄	6 March 2000	list

(317662) 2003 FY₁₂₂	31 March 2003	list
(318601) 2005 JX₄₅	3 May 2005	list
(321876) 2010 SG₇	23 February 2001	list
(337289) 2000 WL₁₉₄	25 November 2000	list
(338450) 2003 EG₅₅	9 March 2003	list
(348151) 2004 FS₁₈	26 March 2004	list
(354650) 2005 JR₄₅	3 May 2005	list
(357315) 2003 FL₁₂₂	31 March 2003	list
(360809) 2005 JH₆₃	3 May 2005	list
(365944) 2012 AZ₁₆	9 March 2003	list
(368103) 2013 EN	3 May 2005	list
(370195) 2002 CU₂₃₁	15 February 2002	list
(370686) 2004 FS₁₂₃	26 March 2004	list
(385437) 2003 GH₅₅	1 April 2003	list
(393559) 2003 GO₃₃	3 April 2003	list
(397214) 2006 GU₃₇	2 April 2006	list
(415789) 2000 WO₁₉₃	24 November 2000	list
(416827) 2005 JU₄₅	3 May 2005	list
(416834) 2005 JY₁₀₈	6 May 2005	list
(416835) 2005 JA₁₀₉	6 May 2005	list
(427831) 2005 JQ₁₀₈	4 May 2005	list
(434011) 2000 YU₁₄₀	19 December 2000	list
(455743) 2005 JV₄₅	3 May 2005	list
(461503) 2003 FJ₁₂₂	31 March 2003	list
(461672) 2005 JM₂₂	6 May 2005	list

(464869) 2005 JL₂₂	4 May 2005	list
(464881) 2005 JF₁₇₇	5 May 2005	list
(468500) 2005 JR₁₀₈	6 May 2005	list
(481053) 2005 JP₄₅	3 May 2005	list

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

^ "Minor Planet Discoverers (by number)". Minor Planet Center. 12 January 2017. Retrieved 2 February 2017.
^ 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. 747 (2) (published March 2012): 6. arXiv:1110.4391. Bibcode:2012ApJ...747L..42D. doi:10.1088/2041-8205/747/2/L42. S2CID 119244278. L42.
^ Chandra X-Ray Observatory (12 April 2012). "DLSCL J0916.2+2951: Discovery of the Musket Ball Cluster". Harvard University.