|
| PAN-STARRS/PS1.g | 4849.11 | 4900.12 | 4810.16 | 3949.50 | 5593.87 | 1053.08 | 3964.03 | 5.05e-9 | PAN-STARRS | PAN-STARRS | PS1 g filter | | PAN-STARRS/PS1.r | 6201.20 | 6241.27 | 6155.47 | 5391.11 | 7038.08 | 1252.41 | 3173.02 | 2.47e-9 | PAN-STARRS | PAN-STARRS | PS1 r filter | | PAN-STARRS/PS1.w | 6285.91 | 6579.22 | 5980.70 | 3986.19 | 8346.21 | 2561.73 | 3231.33 | 2.45e-9 | PAN-STARRS | PAN-STARRS | PS1 w filter | | PAN-STARRS/PS1.open | 6943.76 | 7461.31 | 6431.87 | 3800.00 | 10808.20 | 3985.02 | 3017.13 | 1.88e-9 | PAN-STARRS | PAN-STARRS | PS1 open filter | | PAN-STARRS/PS1.open | Filter Description | Filter ID (?) : | PAN-STARRS/PS1.open |
| Description (?) : | PS1 open filter |
| Phot.System (?) : | PAN-STARRS |
| Detector Type (?) : | Photon counter |
| Band Name (?) : | ------ |
| Obs. Facility (?) : | PAN-STARRS |
| Instrument (?) : | PAN-STARRS |
| Comments (?) : | Including the nominal 1.2 airmasses of the Pan-STARRS1 standard atmospheric extinction. |
| | Mathematical properties | Property | Calculated | Specified | Unit | | λref (?) : |
6943.76 | ------- | (Angstrom) |
| λmean (?) : |
7461.31 | ------- | (Angstrom) |
| λcen (?) : |
7642.33 | ------- | (Angstrom) |
| λeff (?) : |
6431.87 | ------- | (Angstrom) |
| λpeak (?) : |
8670.00 | ------- | (Angstrom) |
| λpivot (?) : |
6943.76 | ------- | (Angstrom) |
| λphot (?) : |
6800.75 | ------- | (Angstrom) |
| λmin (?) : |
3800.00 | ------- | (Angstrom) |
| λmax (?) : |
10808.20 | ------- | (Angstrom) |
| Weff (?) : |
3985.02 | ------- | (Angstrom) |
| FWHM (?) : |
4098.10 | ------- | (Angstrom) |
| Af/AV (?) : |
0.741 | ------- | () |
| Fsun (?) : |
129.79 | ------- | (erg/cm2/s/A) |
| Transmission
Data file: ascii, VOTable Reference for filter response:
U. Hawaii Transmission components: Filter + Instrument + Atmosphereid:PAN-STARRS/PS1.open
You can download here the GaiaXPy base XML file for the full PAN-STARRS/PS1 filter set.
Please, take a look to GaiaXPy documentation for more information. - GaiaXPy base XML file. | | Calibration properties
Vega System | Property | Specified | Calculated | Unit | | Zero Point (?) : |
------- |
1.87597e-9 | (erg/cm2/s/A) |
| |
------- |
3017.13 | (Jy) |
| ZP Type (?) : |
Pogson |
| PhotCal ID (?) : |
PAN-STARRS/PS1.open/Vega |
| |
AB System | Property | Specified | Calculated | Unit | | Zero Point (?) : |
------- |
2.25765e-9 | (erg/cm2/s/A) |
| |
------- |
3631.00 | (Jy) |
| ZP Type (?) : |
Pogson |
| PhotCal ID (?) : |
PAN-STARRS/PS1.open/AB |
| |
ST System | Property | Specified | Calculated | Unit | | Zero Point (?) : |
------- |
3.631e-9 | (erg/cm2/s/A) |
| |
------- |
5839.76 | (Jy) |
| ZP Type (?) : |
Pogson |
| PhotCal ID (?) : |
PAN-STARRS/PS1.open/ST |
| |
|
Filter added: 2015-12-05 13:28:26
Last update: 2021-07-27 20:27:42 | | PAN-STARRS/PS1.i | 7534.96 | 7563.76 | 7503.03 | 6783.17 | 8306.24 | 1206.62 | 2575.36 | 1.36e-9 | PAN-STARRS | PAN-STARRS | PS1 i filter | | PAN-STARRS/PS1.z | 8674.20 | 8690.10 | 8668.36 | 8030.68 | 9350.47 | 997.72 | 2261.81 | 9.01e-10 | PAN-STARRS | PAN-STARRS | PS1 z filter | | PAN-STARRS/PS1.y | 9627.79 | 9644.63 | 9613.60 | 9100.88 | 10877.59 | 638.98 | 2180.40 | 7.05e-10 | PAN-STARRS | PAN-STARRS | PS1 y filter |
| Filter Plots
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 ≡ 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=7461.3104352044&id=PAN-STARRS/PS1.open><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=6431.865942007&id=PAN-STARRS/PS1.open><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=6943.7616548862&id=PAN-STARRS/PS1.open><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=6800.750768629&id=PAN-STARRS/PS1.open><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=3985.0189913126,7642.3343771139,1&id=PAN-STARRS/PS1.open><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}
