HST :The Hubble Space Telescope (HST) is a cooperative program of the European Space Agency (ESA) and the National Aeronautics and Space Administration (NASA) to operate a space-based observatory for the benefit of the international astronomical community. HST/WFC3_IR :The Wide Field Camera 3, IR channel.id:HST/WFC3_IR.a |
| HST/WFC3_IR.F098M | 9862.72 | 9900.03 | 9826.81 | 8894.54 | 10848.68 | 1485.01 | 2136.12 | 6.58e-10 | HST | WFC3 | F098M filter for HST WFC3_IR | | HST/WFC3_IR.G102 | 9989.86 | 10116.70 | 9869.64 | 8000.00 | 11724.79 | 2430.91 | 2074.54 | 6.23e-10 | HST | WFC3 | G102 grism for HST WFC3_IR | | HST/WFC3_IR.G102 | Filter Description | Filter ID (?) : | HST/WFC3_IR.G102 |
| Description (?) : | G102 grism for HST WFC3_IR |
| Phot.System (?) : | WFC3-IR |
| Detector Type (?) : | Photon counter |
| Band Name (?) : | ------ |
| Obs. Facility (?) : | HST |
| Instrument (?) : | WFC3 |
| Comments (?) : | Response calculated at a reference time, June 26, 2009, i.e. approximately when WFC3 was installed on HST. Using filter throughputs determined in the lab in combination with the measured QE of the flight detectors and sensitivities of WFC3's optics.
These values were derived with STsynphot by using filter and correction files from the latest photometric calibration released on October 2020 (Bajaj et al 2020, Calamida et al. 2021). For more information on the latest photometric calibration please see the Photometric calibration webpage.
|
| | Mathematical properties | Property | Calculated | Specified | Unit | | λref (?) : |
9989.86 | ------- | (Angstrom) |
| λmean (?) : |
10116.70 | ------- | (Angstrom) |
| λcen (?) : |
10187.12 | ------- | (Angstrom) |
| λeff (?) : |
9869.64 | ------- | (Angstrom) |
| λpeak (?) : |
11103.04 | ------- | (Angstrom) |
| λpivot (?) : |
9989.86 | ------- | (Angstrom) |
| λphot (?) : |
9955.46 | ------- | (Angstrom) |
| λmin (?) : |
8000.00 | ------- | (Angstrom) |
| λmax (?) : |
11724.79 | ------- | (Angstrom) |
| Weff (?) : |
2430.91 | ------- | (Angstrom) |
| FWHM (?) : |
2590.40 | ------- | (Angstrom) |
| Af/AV (?) : |
0.429 | ------- | () |
| Fsun (?) : |
72.26 | ------- | (erg/cm2/s/A) |
| Transmission
Data file: ascii, VOTable Reference for filter response:
Wide Field Camera 3 Performance Transmission components: Filter + CCD + Instrumentid:HST/WFC3_IR.G102 | | Calibration properties
Vega System | Property | Specified | Calculated | Unit | | Zero Point (?) : |
------- |
6.23195e-10 | (erg/cm2/s/A) |
| |
------- |
2074.54 | (Jy) |
| ZP Type (?) : |
Pogson |
| PhotCal ID (?) : |
HST/WFC3_IR.G102/Vega |
| |
AB System | Property | Specified | Calculated | Unit | | Zero Point (?) : |
------- |
1.09076e-9 | (erg/cm2/s/A) |
| |
------- |
3631.00 | (Jy) |
| ZP Type (?) : |
Pogson |
| PhotCal ID (?) : |
HST/WFC3_IR.G102/AB |
| |
ST System | Property | Specified | Calculated | Unit | | Zero Point (?) : |
------- |
3.631e-9 | (erg/cm2/s/A) |
| |
------- |
12087.16 | (Jy) |
| ZP Type (?) : |
Pogson |
| PhotCal ID (?) : |
HST/WFC3_IR.G102/ST |
| |
|
Filter added: 2019-07-16 12:15:40
Last update: 2022-03-01 15:27:10 | | HST/WFC3_IR.F105W | 10550.25 | 10651.00 | 10430.83 | 8955.24 | 12130.55 | 2371.97 | 1974.81 | 5.32e-10 | HST | WFC3 | F105W filter for HST WFC3_IR | | HST/WFC3_IR.F110W | 11534.46 | 11797.14 | 11200.52 | 8845.79 | 14122.58 | 3856.85 | 1775.57 | 4.0e-10 | HST | WFC3 | F110W filter for HST WFC3_IR | | HST/WFC3_IR.F125W | 12486.07 | 12576.18 | 12363.55 | 10853.22 | 14141.73 | 2674.40 | 1555.41 | 2.99e-10 | HST | WFC3 | F125W filter for HST WFC3_IR | | HST/WFC3_IR.F126N | 12585.43 | 12585.67 | 12585.05 | 12481.60 | 12692.56 | 149.85 | 1524.51 | 2.89e-10 | HST | WFC3 | F126N filter for HST WFC3_IR | | HST/WFC3_IR.F127M | 12741.07 | 12746.22 | 12732.37 | 12268.83 | 13235.27 | 673.44 | 1469.99 | 2.71e-10 | HST | WFC3 | F127M filter for HST WFC3_IR | | HST/WFC3_IR.F128N | 12836.65 | 12837.00 | 12837.23 | 12729.50 | 12947.67 | 157.47 | 1366.21 | 2.49e-10 | HST | WFC3 | F128N filter for HST WFC3_IR | | HST/WFC3_IR.F130N | 13010.38 | 13010.63 | 13010.12 | 12904.91 | 13116.80 | 154.57 | 1448.43 | 2.57e-10 | HST | WFC3 | F130N filter for HST WFC3_IR | | HST/WFC3_IR.F132N | 13193.46 | 13193.72 | 13193.12 | 13084.22 | 13302.38 | 158.69 | 1419.26 | 2.44e-10 | HST | WFC3 | F132N filter for HST WFC3_IR | | HST/WFC3_IR.F139M | 13841.81 | 13846.00 | 13836.06 | 13403.18 | 14303.22 | 630.71 | 1317.21 | 2.06e-10 | HST | WFC3 | F139M filter for HST WFC3_IR | | HST/WFC3_IR.F140W | 13923.21 | 14061.91 | 13734.66 | 11864.94 | 16133.14 | 3569.86 | 1321.43 | 2.04e-10 | HST | WFC3 | F140W filter for HST WFC3_IR | | HST/WFC3_IR.G141 | 13886.72 | 14184.79 | 13477.70 | 10436.79 | 17780.13 | 4917.01 | 1355.32 | 2.11e-10 | HST | WFC3 | G141 grism for HST WFC3_IR | | HST/WFC3_IR.F153M | 15332.75 | 15336.98 | 15326.28 | 14869.68 | 15828.81 | 692.30 | 1119.04 | 1.43e-10 | HST | WFC3 | F153M filter for HST WFC3_IR | | HST/WFC3_IR.F160W | 15370.34 | 15436.30 | 15278.47 | 13857.70 | 17003.09 | 2750.15 | 1122.80 | 1.42e-10 | HST | WFC3 | F160W filter for HST WFC3_IR | | HST/WFC3_IR.F164N | 16449.96 | 16450.31 | 16451.45 | 16308.82 | 16591.89 | 206.74 | 983.46 | 1.09e-10 | HST | WFC3 | F164N filter for HST WFC3_IR | | HST/WFC3_IR.F167N | 16676.00 | 16676.59 | 16674.00 | 16533.47 | 16821.47 | 208.88 | 1006.74 | 1.09e-10 | HST | WFC3 | F167N filter for HST WFC3_IR |
|
| 
 ≡ 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=10116.696202465&id=HST/WFC3_IR.G102><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=9869.6409644487&id=HST/WFC3_IR.G102><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=9989.8601157007&id=HST/WFC3_IR.G102><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=9955.4590937892&id=HST/WFC3_IR.G102><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=2430.907460434,10187.116841024,1&id=HST/WFC3_IR.G102><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}
