The following filters are now available in the full 5.75 inch size required for the Mosaic CCD imagers. If you would like to bring your own filters, the physical size should be 146 x 146 mm, and the filter should be 12 mm thick. Properties for the CTIO interference filters shown below are at the f/2.9 of the CTIO 4-m prime focus. Properties shown below for the 4meter filters are for parallel light. Note that most KPNO Mosaic filters (except for the U filter) are parfocal while at CTIO the filters are NOT parfocal - approximate focus offsets can be found on the CTIO Mosaic filters page.
As of April 24, 2012 all CTIO Mosaic-2 filters have been transferred to KPNO and are available for use with Mosaic-1.
For more information on a filter (e.g. to view transmission curves), click on the filter name. All KPNO Mosaic filters were measured at NOAO.
||Central Wave, Å||FWHM, Å||Peak Trans||
||Central Wave, Å||FWHM, Å||Peak Trans|
|U k1001||3552||630.71||76.39%||U c6001||3570||650||72.47%|
|B Harris k1002||4381||993.88||69.62%||B Harris c6002||4360||990||62.8%|
|V Harris k1003||5386.76||948.66||88.62%||V Harris c6026||5370||940||87.61%|
|R Harris k1004||6513.54||1511.3||86.86%||R Harris c6004||6440||1510||81.98%|
|I Nearly-Mould k1005||8204.53||1914.59||94.82%||I c6028||8050||1500||95.74%|
|C Washington k1006||3860||1034||75.4%||C Washington c6029||3850||1075||83%|
|M Washington k1007||5100||1140||87.1%||M Washington c6007||5020||1020||90.75%|
|D51 DDO 51 k1008||5145.2||162.9||87.56%||D51 DDO 51 c6008||5130||154||84.76%|
|ha H-alpha k1009||6574.74||80.62||94.31%||ha H-alpha c6009||6563||80||75.87%|
|ha4 H-alpha+4nm k1010||6620.52||80.48||91.81%||ha8 H-alpha+8nm c6011||6650||80||86.24%|
|ha8 H-alpha+8nm k1011||6654.19||81.33||90.58%||o2 OII c6012||3727||50||61.12%|
|ha12 H-alpha+12nm k1012||6698.53||82.95||86.43%||s2 SII c6013||6725||80||74.03%|
|ha16 H-alpha+16nm k1013||6730.72||81.1||91.12%||o3 OIII c6014||4990||50||74.09%|
|O3 OIII N2 k1014 *||5024.9||55.55||76.48%||wh Bk-7 c6016||6500||5000|
|Ooff OIII+30nm k1015||5317.54||242.69||92.79%||g SDSS c6017||4813||1537||89.34%|
|wh Bk-7 k1016||5600||6800||97.2%||r SDSS c6018||6287||1468||93.82%|
|g SDSS k1017||4750.58||1395.73||91.16%||i SDSS c6019||7732||1548||93.55%|
|r SDSS k1018||6292.28||1475.17||92.83%||z SDSS c6020||9400||2000||99.94%|
|i SDSS k1019||7726.28||1539.89||95.17%||u SDSS c6022||3600||400||65.49%|
|z SDSS k1020 *** Retired!||9400||2000||94.8%||Bj Tyson c6024||4350||1650||85.1%|
|wrc3 WR CIII k1021||4666.15||51.71||71.5%||It Tyson I c6025||8800||2000||99.61%|
|wr475 WR 475 k1022||4764||51.27||82.19%||VR Stubbs c6027||6100||2000||89.6%|
|wrhe2 WR HeII k1023||4702.6||50.31||80.72%|
|wrc4 WR CIV k1024||5828.71||41.79||74.8%|
|Bw NDWFS k1025||4110.78||1275.21||93.88%|
|815 815_v1 k1026||8152.10||70.36||96.21%|
|823 823_v1 k1027||8232.04||70.61||96.11%|
|918R 918R_v1 k1028||9210.96||81.22||90.06%|
|VR Bernstein k1040 *** Retired!||5944.95||2119.56||95.40%|
|Un Steidel k1041||3479.17||562.72||81.47%|
|Gn Steidel k1042||4819.66||762.13||89.38%|
|Rs Steidel k1043||6975.13||1048.78||90.11%|
|Us solid U k1044||3651.81||588.20||81.15%|
|Ud Dey custom U k1045||3485.23||329.76||73.16%|
|815 815_v2 k1046||8152.64||68.53||84.52%|
|823 823_v2 k1047||8238.79||68.02||92.74%|
|337 BATC k1051 **||54.97%|
|390 BATC k1052 **||58.40%|
|420 BATC k1053 **||64.03%|
|454 BATC k1054 **||81.80%|
|493 BATC k1055 **||87.41%|
|527 BATC k1056 **||84.57%|
|579 BATC k1057 **||88.91%|
|607 BATC k1058 **||87.31%|
|666 BATC k1059 **||87.14%|
|705 BATC k1060 **||83.80%|
|755 BATC k1061 **||78.25%|
|802 BATC k1062 **||85.86%|
|848 BATC k1063 **||88.35%|
|918 BATC k1064 **||80.00%|
|973 BATC k1065 **||84.08%|
Below are plots of some of our filter sets. Click on the plot to view full size.
* The [OIII] filter is not a good match for the 0.9-m -- a replacement has been proven difficult to construct. For now, there are no alternatives.
** Rogier Windhorst and collaborators at Arizona State University are making available to users of MOSAIC-1 at the Mayall 4m telescope and NOAO time on the WIYN 0.9m telescope 15 medium band filters designed to avoid the brightest and most variable night sky lines. The September 2001 issue of the NOAO newsletter (see page 34) contains an article describing the filters along with references describing their past use by Windhorst and collaborators. A figure showing the throughput curves for the filters is available via the link below. The entire ASU/Windhorst filter set includes 15 filters covering from 3370 angstroms to 9730 angstroms. The filters "Windhorst XXXXXXX a" through "Windhorst XXXXX p" in the above list of Mosaic filters (by serial number these are k1051 through k1065 in the list) can be requested for use.
The BATC filter set belongs to Dr. Rogier Windhorst of Arizona State University. Observers wishing to use these filters should request permission to use these filters from Dr. Windhorst (Rogier.Windhorst@asu.edu) prior to submitting their proposals to the NOAO TAC. Dr. Windhorst will inform NOAO when he has given approval for use of the filter. Please make clear in your request to Dr. Windhorst the following information: Proposed Telescope/Instrument; PI of intended proposal; General Science goals of the proposal.
Rogier Windhorst has provided the following figure showing the transmission of the ASU/Windhorst filter set, Click Here. Note that the filters are labeled a through k, m through p, these short "letter" names will allow you to match the filters to the wavelength name. For example, "a" corresponds to filter "337 BATC", etc..
*** The KPNO VR Berstein and KPNO SDSS z' filters were damaged in June 2011. The CTIO equivalents (VR Stubbs, c6027 and SDSS z', c6020) can be requested as replacements.