Roman :The Roman Space Telescope is a NASA observatory designed to unravel the secrets of dark energy and dark matter, search for and image exoplanets, and explore many topics in infrared astrophysics. Roman/WFI :The Wide-Field Instrument (WFI) is the primary instrument of the Roman Space Telescope. WFI provides wide-field imaging and multi-object, slitless spectroscopy over an. 0.281 deg2 field-of-view.id:Roman/WFI.a |
| Roman/WFI.F062 | 6290.80 | 6434.12 | 6141.54 | 4633.82 | 7888.11 | 2122.29 | 3174.18 | 2.4e-9 | Roman | WFI | Roman WFI F062 filter eff. area. | | Roman/WFI.F087 | 8695.98 | 8764.83 | 8650.97 | 7328.23 | 10133.08 | 1892.17 | 2294.04 | 9.09e-10 | Roman | WFI | Roman WFI F087 filter eff. area. | | Roman/WFI.F106 | 10566.52 | 10652.07 | 10465.04 | 8938.32 | 12357.27 | 2440.85 | 1967.08 | 5.28e-10 | Roman | WFI | Roman WFI F106 filter eff. area. | | Roman/WFI.F129 | 12901.34 | 13005.01 | 12759.99 | 10907.72 | 15074.53 | 2939.26 | 1483.60 | 2.67e-10 | Roman | WFI | Roman WFI F129 filter eff. area. | | Roman/WFI.F129 | Filter Description | Filter ID (?) : | Roman/WFI.F129 |
| Description (?) : | Roman WFI F129 filter eff. area. |
| Phot.System (?) : | WFI |
| Detector Type (?) : | Photon counter |
| Band Name (?) : | ------ |
| Obs. Facility (?) : | Roman |
| Instrument (?) : | WFI |
| Comments (?) : | ------ |
| | Mathematical properties | Property | Calculated | Specified | Unit | | λref (?) : |
12901.34 | ------- | (Angstrom) |
| λmean (?) : |
13005.01 | ------- | (Angstrom) |
| λcen (?) : |
12952.44 | ------- | (Angstrom) |
| λeff (?) : |
12759.99 | ------- | (Angstrom) |
| λpeak (?) : |
14100.00 | ------- | (Angstrom) |
| λpivot (?) : |
12901.34 | ------- | (Angstrom) |
| λphot (?) : |
12829.12 | ------- | (Angstrom) |
| λmin (?) : |
10907.72 | ------- | (Angstrom) |
| λmax (?) : |
15074.53 | ------- | (Angstrom) |
| Weff (?) : |
2939.26 | ------- | (Angstrom) |
| FWHM (?) : |
3191.06 | ------- | (Angstrom) |
| Af/AV (?) : |
0.283 | ------- | () |
| Fsun (?) : |
41.54 | ------- | (erg/cm2/s/A) |
| Effective area
Data file: ascii, VOTable Reference for filter response:
Wide-Field Instrument : Technical Transmission components: Filter + CCD + Instrumentid:Roman/WFI.F129 | | Calibration properties
Vega System | Property | Specified | Calculated | Unit | | Zero Point (?) : |
------- |
2.67219e-10 | (erg/cm2/s/A) |
| |
------- |
1483.60 | (Jy) |
| ZP Type (?) : |
Pogson |
| PhotCal ID (?) : |
Roman/WFI.F129/Vega |
| |
AB System | Property | Specified | Calculated | Unit | | Zero Point (?) : |
------- |
6.53999e-10 | (erg/cm2/s/A) |
| |
------- |
3631.00 | (Jy) |
| ZP Type (?) : |
Pogson |
| PhotCal ID (?) : |
Roman/WFI.F129/AB |
| |
ST System | Property | Specified | Calculated | Unit | | Zero Point (?) : |
------- |
3.631e-9 | (erg/cm2/s/A) |
| |
------- |
20159.29 | (Jy) |
| ZP Type (?) : |
Pogson |
| PhotCal ID (?) : |
Roman/WFI.F129/ST |
| |
|
Filter added: 2023-02-01 11:57:24
Last update: 2023-02-01 11:57:24 | | Roman/WFI.Prism | 12499.08 | 13584.80 | 11229.66 | 7403.20 | 18230.22 | 7168.79 | 1683.10 | 3.23e-10 | Roman | WFI | Roman WFI Prism eff. area. | | Roman/WFI.Grism | 14246.69 | 14885.70 | 13416.28 | 9950.28 | 19394.91 | 7843.92 | 1355.34 | 2.0e-10 | Roman | WFI | Roman WFI Grism eff. area. | | Roman/WFI.F146 | 14377.83 | 15378.47 | 13049.63 | 8957.65 | 20731.99 | 7889.83 | 1396.74 | 2.03e-10 | Roman | WFI | Roman WFI F146 filter eff. area. | | Roman/WFI.F158 | 15748.67 | 15875.37 | 15577.83 | 13310.97 | 18389.02 | 3546.72 | 1091.96 | 1.32e-10 | Roman | WFI | Roman WFI F158 filter eff. area. | | Roman/WFI.F184 | 18394.10 | 18466.13 | 18290.96 | 16227.63 | 20732.13 | 3022.52 | 854.12 | 7.57e-11 | Roman | WFI | Roman WFI F184 filter eff. area. | | Roman/WFI.F213 | 21229.96 | 21306.18 | 21116.87 | 18805.31 | 23835.10 | 3338.65 | 675.72 | 4.49e-11 | Roman | WFI | Roman WFI F213 filter eff. area. |
|
| 
 ≡ filter transmission<p><u>Property info:</u><ul><li><b>Unit</b>:Angstrom<li><b>UCD</b>:em.wl</ul></td></table>',WIDTH,400)){kind=link}
 ≡ filter transmission<br> Vg(λ) ≡ Vega spectrum.<p><u>More info:</u><p>Vega spectrum from calspec database.<ul><li><a href="https://ui.adsabs.harvard.edu/abs/2014PASP..126..711B/abstract" target="_blank">Bohlin, Gordon, & Tremblay (2014)</a>.<li><a href="https://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogs/calspec" target="_blank">STScI current calspec</a>.<li><a href="morefiles/vega.dat" target="_blank">Vega spectrum file</a> (units: Angstrom erg/cm2/s/A).</ul><p><u>Property info:</u><ul><li><b>Unit</b>:Angstrom<li><b>UCD</b>:em.wl.effective</ul></td></table>',WIDTH,400)){kind=link}
 ≡ filter transmission<p>Equivalent to the horizontal size of a rectangle with height equal to maximum transmission and with the same area that the one covered by the filter transmission curve.<p><u>Property info:</u><ul><li><b>Unit</b>:Angstrom<li><b>UCD</b>:instr.bandwidth<li><b>Utype</b>: <i>photdm:PhotometryFilter.bandwidth.extent.value</i></ul></td></table>',WIDTH,400)){kind=link}
 ≡ filter transmission (energy counter).<br> Vg(λ) ≡ Vega spectrum.<p><i>(T(λ) must be multiplied by λ for photon counting devices)</i><p>F<sub>0,ν</sub>(Jy) = (2.9979246)<sup>-1</sup> 10<sup>5</sup> * λ<sub>ref</sub><sup>2</sup> * F<sub>0,λ</sub>(erg/cm<sup>2</sup>/s/A)<p>In the case that filter owner specifies its own values, they will be the ones provided by the service when queried through the VO.<p><u>Property info:</u><ul><li><b>Unit</b>:Jy<li><b>UCD</b>:phot.flux.density<li><b>Utype</b>: <i>photdm:PhotCal.zeroPoint.flux.value</i></ul></td></table>',WIDTH,400)){kind=link}
 ≡ filter transmission (energy counter).<br> Vg(λ) ≡ Vega spectrum.<p><i>(T(λ) must be multiplied by λ for photon counting devices)</i><p><u>Property info:</u><ul><li><b>Unit</b>:erg/cm2/s/A<li><b>Utype</b>: <i>PhotCal.ZeroPoint</i></ul></td></table>',WIDTH,400)){kind=link}
 ≡ filter transmission<p>f(λ) ≡ flux of the spectrum<p><u>Property info:</u><ul><li><b>UCD</b>:meta.code<li><b>Utype</b>: <i>photdm:PhotometricSystem.detectorType</i></ul></td></table>',WIDTH,400)){kind=link}
 ≡ filter transmission<p><img src=showgraph.php?what=lmean&val=13005.009424876&id=Roman/WFI.F129><p>Filter transmission is transformed to "<i>energy counter</i>" for these calculations, that is, the photon count transmission is multiplied by λ and normalized so that peak transmission is equal to 1.<p><u>Property info:</u><ul><li><b>Unit</b>:Angstrom<li><b>UCD</b>:em.wl</ul></td></table>',STICKY,true,CLOSEBTN,true,WIDTH,400)){kind=link}
 ≡ filter transmission<br> Vg(λ) ≡ Vega spectrum.<p><img src=showgraph.php?what=leff&val=12759.987197588&id=Roman/WFI.F129><p>Filter transmission is transformed to "<i>energy counter</i>" for these calculations, that is, the photon count transmission is multiplied by λ and normalized so that peak transmission is equal to 1.<p><u>More info:</u><p>Vega spectrum from calspec database.<ul><li><a href="https://ui.adsabs.harvard.edu/abs/2014PASP..126..711B/abstract" target="_blank">Bohlin, Gordon, & Tremblay (2014)</a>.<li><a href="https://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogs/calspec" target="_blank">STScI current calspec</a>.<li><a href="morefiles/vega.dat" target="_blank">Vega spectrum file</a> (units: Angstrom erg/cm2/s/A).</ul><p><u>Property info:</u><ul><li><b>Unit</b>:Angstrom<li><b>UCD</b>:em.wl.effective</ul></td></table>',STICKY,true,CLOSEBTN,true,WIDTH,400)){kind=link}
 ≡ filter transmission<p><img src=showgraph.php?what=lpiv&val=12901.339349728&id=Roman/WFI.F129><p>Filter transmission is transformed to "<i>energy counter</i>" for these calculations, that is, the photon count transmission is multiplied by λ and normalized so that peak transmission is equal to 1.<p><u>Property info:</u><ul><li><b>Unit</b>:Angstrom<li><b>UCD</b>:em.wl</ul></td></table>',STICKY,true,CLOSEBTN,true,WIDTH,400)){kind=link}
 ≡ filter transmission<br> Vg(λ) ≡ Vega spectrum<p><img src=showgraph.php?what=lphot&val=12829.122119187&id=Roman/WFI.F129><p>Filter transmission is transformed to "<i>energy counter</i>" for these calculations, that is, the photon count transmission is multiplied by λ and normalized so that peak transmission is equal to 1.<p><u>More info:</u><p>Vega spectrum from calspec database.<ul><li><a href="https://ui.adsabs.harvard.edu/abs/2014PASP..126..711B/abstract" target="_blank">Bohlin, Gordon, & Tremblay (2014)</a>.<li><a href="https://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogs/calspec" target="_blank">STScI current calspec</a>.<li><a href="morefiles/vega.dat" target="_blank">Vega spectrum file</a> (units: Angstrom erg/cm2/s/A).</ul><p><u>Property info:</u><ul><li><b>Unit</b>:Angstrom<li><b>UCD</b>:em.wl</ul></td></table>',STICKY,true,CLOSEBTN,true,WIDTH,400)){kind=link}
 ≡ filter transmission<p>Equivalent to the horizontal size of a rectangle with height equal to maximum transmission and with the same area that the one covered by the filter transmission curve.<p><img src=showgraph.php?what=weff&val=2939.2594447114,12952.437250029,1&id=Roman/WFI.F129><p>Filter transmission is transformed to "<i>energy counter</i>" for these calculations, that is, the photon count transmission is multiplied by λ and normalized so that peak transmission is equal to 1.<p><u>Property info:</u><ul><li><b>Unit</b>:Angstrom<li><b>UCD</b>:instr.bandwidth<li><b>Utype</b>: <i>photdm:PhotometryFilter.bandwidth.extent.value</i></ul></td></table>',STICKY,true,CLOSEBTN,true,WIDTH,400)){kind=link}
![(?)](javascript:Tip('<b>A<sub>f</sub>/A<sub>V</sub></b><br><table cellpadding=20><td class=helptd>Ratio between extintion at λ<sub>ref</sub> and visual extintion. <p>Calculated by the service using the extinction law by <a href="http://adsabs.harvard.edu/abs/1999PASP..111...63F" target="_blank">Fitzpatrick (1999)</a> improved by <a href="http://adsabs.harvard.edu/abs/2005ApJ...619..931I" target="_blank">Indebetouw et al (2005)</a> in the infrared. <p><img src="images/extlaw.png"><p>You can download the corresponding <a href=\"getextlaw.php\" target=\"_blank\">data file</a> for the opacity k<sub>λ</sub>. The extinction at each wavelength is calculated as: A<sub>λ</sub> = A<sub>V</sub> * k<sub>λ</sub>/k<sub>V</sub>, where k<sub>λ</sub> is the opacity for a given λ and k<sub>V</sub>=211.4<p><p><u>Property info:</u><ul></ul></td></table>',STICKY,true,CLOSEBTN,true,WIDTH,400)){kind=link}
 ≡ filter transmission.<br> Sun(λ) ≡ Sun spectrum.<p><img src="images/sun.png"><p><p>Filter transmission is transformed to "<i>energy counter</i>" for these calculations, that is, the photon count transmission is multiplied by λ and normalized so that peak transmission is equal to 1.<p><u>More info:</u><p>Sun spectrum from calspec database: sun_reference_stis_002 composed with sun_mod_001 for larger wavelengths.<ul><li><a href="https://ui.adsabs.harvard.edu/abs/2014PASP..126..711B/abstract" target="_blank">Bohlin, Gordon, & Tremblay (2014)</a>.<li><a href="https://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogs/calspec" target="_blank">STScI current calspec</a>.<li><a href="morefiles/sun.dat" target="_blank">Sun composed spectrum</a> (units: Angstrom erg/cm2/s/A).</ul><p><u>Property info:</u><ul><li><b>Unit</b>:erg/cm2/s/A<li><b>UCD</b>:phot.flux.density</ul></td></table>',STICKY,true,CLOSEBTN,true,WIDTH,400)){kind=link}
 ≡ filter transmission.<br> Vg(λ) ≡ Vega spectrum.<p>F<sub>0,ν</sub>(Jy) = (2.9979246)<sup>-1</sup> 10<sup>5</sup> * λ<sub>ref</sub><sup>2</sup> * F<sub>0,λ</sub>(erg/cm<sup>2</sup>/s/A)<p>Filter transmission is transformed to \"<i>energy counter</i>\" for these calculations, that is, the photon count transmission is multiplied by λ and normalized so that peak transmission is equal to 1.<p>In the case that filter owner specifies its own values, they will be the ones provided by the service when queried through the VO.<p><u>VO PhotDM Utypes</u>: <br><i>PhotCal.MagnitudeSystem.type</i> -> VEGAmag <br><i>PhotCal.ZeroPoint.Flux.value</i> -> F<sub>0</sub><p><u>More info:</u><p>Vega spectrum from calspec database.<ul><li><a href="https://ui.adsabs.harvard.edu/abs/2014PASP..126..711B/abstract" target="_blank">Bohlin, Gordon, & Tremblay (2014)</a>.<li><a href="https://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogs/calspec" target="_blank">STScI current calspec</a>.<li><a href="morefiles/vega.dat" target="_blank">Vega spectrum file</a> (units: Angstrom erg/cm2/s/A).</ul><p><u>Property info:</u><ul><li><b>UCD</b>:phot.flux.density<li><b>Utype</b>: <i>photdm:PhotCal.ZeroPoint.Flux.value</i></ul></td></table>',STICKY,true,CLOSEBTN,true,WIDTH,400)){kind=link}
