Difference between revisions of "Hauptseite"
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'''Important: '''We are recovering after and attack and things will take time for full functionality. | '''Important: '''We are recovering after and attack and things will take time for full functionality. | ||
| − | You can find the entire Lightmeter wiki for reading only at [http://kuffner-sternwarte.at/hms/wiki | + | You can find the entire Lightmeter wiki for reading only at [http://kuffner-sternwarte.at/hms/wiki/ http://kuffner-sternwarte.at/hms] |
[[File:JP Setagaya 1 Jun-Dec 2012 distribution.png|right|800px|Distribution of the total radiatio - the light at night - in 2012 at the Setagaya - Tokyo Lightmeter station Details of the Setagaya station at the GAVO Lightmeter data-centre. The distribution of the decadic logarithm of total radiation in Watt per squaere meter W/m² is are shown as measured from June to December 2012 (courtesy Nobuaki Ochi and the Setagaya station.]] | [[File:JP Setagaya 1 Jun-Dec 2012 distribution.png|right|800px|Distribution of the total radiatio - the light at night - in 2012 at the Setagaya - Tokyo Lightmeter station Details of the Setagaya station at the GAVO Lightmeter data-centre. The distribution of the decadic logarithm of total radiation in Watt per squaere meter W/m² is are shown as measured from June to December 2012 (courtesy Nobuaki Ochi and the Setagaya station.]] | ||
| − | [[File:Lightmeter Teide observatory.jpeg|thumb | + | [[File:Lightmeter Teide observatory.jpeg|thumb]] |
| − | [[File:Lightmeter 1Euro persp.png|thumb | + | [[File:Lightmeter 1Euro persp.png|thumb]] |
| − | [[File:Juni2009 Linz Wien Berlin Tautenburg.png|thumb | + | [[File:Juni2009 Linz Wien Berlin Tautenburg.png|thumb]] |
| − | [[File:Juni 12bis17 2009 Berlin Tautenburg.png|thumb | + | [[File:Juni 12bis17 2009 Berlin Tautenburg.png|thumb]] |
'''Goal:''' To continuously measure the state of the world's nightskies with a global network of low-cost lightmeters in the year of astronomy and to start the long-term monitoring of light pollution on Earth. | '''Goal:''' To continuously measure the state of the world's nightskies with a global network of low-cost lightmeters in the year of astronomy and to start the long-term monitoring of light pollution on Earth. | ||
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=== Mark 2.3 IYA - International Year of Astronome series === | === Mark 2.3 IYA - International Year of Astronome series === | ||
| − | [[File:Mark 2.3 Lightmeter.jpg|thumb | + | [[File:Mark 2.3 Lightmeter.jpg|thumb]] |
With the extra linear "daylight" Lux-oriented eye. This additional two channel sensor assists in calibrating the non-linear daylight range of the instrument and can be used to directly compare to Lux values as it is manufacturer calibrated and its output can be directly converted to illumination (see the driver section). | With the extra linear "daylight" Lux-oriented eye. This additional two channel sensor assists in calibrating the non-linear daylight range of the instrument and can be used to directly compare to Lux values as it is manufacturer calibrated and its output can be directly converted to illumination (see the driver section). | ||
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=== Hardware (Mark 2 original series prototype) === | === Hardware (Mark 2 original series prototype) === | ||
| − | [[File:Lightmeter packshot.jpg|thumb | + | [[File:Lightmeter packshot.jpg|thumb]] |
*solar-cell in Aluminium frame with closed electronics. | *solar-cell in Aluminium frame with closed electronics. | ||
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= Lightmeter performance = | = Lightmeter performance = | ||
| − | [[File:L12 31March2009png.png|thumb | + | [[File:L12 31March2009png.png|thumb]] |
The lightmeter measures fully automatic and up to 20 times per second. Measurmeents are recorded with an adjustable rate of up to once per second and are stored in a .csv or text file with fixes column width that can be easily read with standard spreadsheet software. Nighttime measurements are done in a linear mode that can be easily converted to approximate Lux-values or received energy per unit surface, like [W/m2] that can be readily related to the energy input by the Sun. To directly measure the Sun a non-linear (approximately logarithmic) daylight range operates at brightness levels above the full moon. This allows to compare daylight and nighttime variations. Alltogether the lightmeter measures from a few 100 000 Lux to 100 mikro-Lux,thus covering 11 orders of magnitude, almost as many as the human eye. | The lightmeter measures fully automatic and up to 20 times per second. Measurmeents are recorded with an adjustable rate of up to once per second and are stored in a .csv or text file with fixes column width that can be easily read with standard spreadsheet software. Nighttime measurements are done in a linear mode that can be easily converted to approximate Lux-values or received energy per unit surface, like [W/m2] that can be readily related to the energy input by the Sun. To directly measure the Sun a non-linear (approximately logarithmic) daylight range operates at brightness levels above the full moon. This allows to compare daylight and nighttime variations. Alltogether the lightmeter measures from a few 100 000 Lux to 100 mikro-Lux,thus covering 11 orders of magnitude, almost as many as the human eye. | ||
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= Calibration = | = Calibration = | ||
| − | [[File:SQM and Luxmeters TLS 18Sep2008 med.png|thumb | + | [[File:SQM and Luxmeters TLS 18Sep2008 med.png|thumb]] |
The lightmeter puts out numbers that are basically the number of electrons that are created by the light-particles when they hit the sensor and are then counted by the electronics. To get from that number or ''counts'' to a standardised quantity like received Energy per Area (Watt/square meter or in short: W/m2) or Illumination (how much much the Sensor is illuminated) in Lux, or short lx you need a ''calibration'' that converts the counts in the standardised measurement quantity in the SI-system. The calibration is usually a factor that has to be multiplied onto the counts that your lightmeter puts out. The standard calibration values to obtain a proxy for the measurement in Lux for the linear night-mode are: | The lightmeter puts out numbers that are basically the number of electrons that are created by the light-particles when they hit the sensor and are then counted by the electronics. To get from that number or ''counts'' to a standardised quantity like received Energy per Area (Watt/square meter or in short: W/m2) or Illumination (how much much the Sensor is illuminated) in Lux, or short lx you need a ''calibration'' that converts the counts in the standardised measurement quantity in the SI-system. The calibration is usually a factor that has to be multiplied onto the counts that your lightmeter puts out. The standard calibration values to obtain a proxy for the measurement in Lux for the linear night-mode are: | ||
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= Conversion of light measurements = | = Conversion of light measurements = | ||
| − | [[File:Grenzgroesse und Beleuchtungsstaerke Tautenburg 2008.png|thumb | + | [[File:Grenzgroesse und Beleuchtungsstaerke Tautenburg 2008.png|thumb]] |
Measurement of the lightmeter can be expressed in various quantities as illumination, the energy flux received by the instrument or the corresponding brightness of the sky or astronomical quantities like the mean brightness per unit area on the sky, for example in magnitudes per square arc-seconds that the Sky Quality Meter puts out. | Measurement of the lightmeter can be expressed in various quantities as illumination, the energy flux received by the instrument or the corresponding brightness of the sky or astronomical quantities like the mean brightness per unit area on the sky, for example in magnitudes per square arc-seconds that the Sky Quality Meter puts out. | ||
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<br/>The lowest detectable signal is estimated to be the light of a single bright star as Sirus. | <br/>The lowest detectable signal is estimated to be the light of a single bright star as Sirus. | ||
| − | [[File:Mueller Mark2.1 L0.3-linearity.jpg|thumb | + | [[File:Mueller Mark2.1 L0.3-linearity.jpg|thumb]] |
The measurement range above the full moon has been added to compare the daylight variations to the nighttime variations. This part is experimental and non-linear. That means twice the counts do not correspond to twice the light. These measurments have to be processed to give physical quantities correcly. | The measurement range above the full moon has been added to compare the daylight variations to the nighttime variations. This part is experimental and non-linear. That means twice the counts do not correspond to twice the light. These measurments have to be processed to give physical quantities correcly. | ||
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Please upload your data! Instructions: [[Lightmeter-database]]. | Please upload your data! Instructions: [[Lightmeter-database]]. | ||
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'''Talks and articles:''' | '''Talks and articles:''' | ||
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'''MediaWiki wurde erfolgreich installiert.''' | '''MediaWiki wurde erfolgreich installiert.''' | ||
| − | <br/>Hilfe zur Benutzung und Konfiguration der Wiki-Software findest du im [[[[[[[[[[//meta.wikimedia.org/wiki/Help:Contents|Benutzerhandbuch||||||||[1]]]]]]]]]]]. | + | <br/>Hilfe zur Benutzung und Konfiguration der Wiki-Software findest du im [[[[[[[[[[[//meta.wikimedia.org/wiki/Help:Contents|Benutzerhandbuch|||||||||[1]]]]]]]]]]]]. |
== Starthilfen == | == Starthilfen == | ||
| − | *[[[[[[[[[[//www.mediawiki.org/wiki/Manual:Configuration_settings|Liste|der|Konfigurationsvariablen||||||[1]]]]]]]]]]] | + | *[[[[[[[[[[[//www.mediawiki.org/wiki/Manual:Configuration_settings|Liste|der|Konfigurationsvariablen|||||||[1]]]]]]]]]]]] |
| − | *[[[[[[[[[[//www.mediawiki.org/wiki/Manual:FAQ|MediaWiki-FAQ||||||||[2]]]]]]]]]]] | + | *[[[[[[[[[[[//www.mediawiki.org/wiki/Manual:FAQ|MediaWiki-FAQ|||||||||[2]]]]]]]]]]]] |
*[https://lists.wikimedia.org/mailman/listinfo/mediawiki-announce Mailingliste neuer MediaWiki-Versionen] | *[https://lists.wikimedia.org/mailman/listinfo/mediawiki-announce Mailingliste neuer MediaWiki-Versionen] | ||
| − | *[[[[[[[[[[//www.mediawiki.org/wiki/Localisation#Translation_resources|Lokalisiere|MediaWiki|für|deine|Sprache||||[1]]]]]]]]]]] | + | *[[[[[[[[[[[//www.mediawiki.org/wiki/Localisation#Translation_resources|Lokalisiere|MediaWiki|für|deine|Sprache|||||[1]]]]]]]]]]]] |
Revision as of 14:29, 29 May 2014
Contents
- 1 This is Starlight and Lightmeter Wiki - new Version after upgrade
- 2 News
- 3 Description of the Lightmeter
- 4 How to get a Lightmeter
- 5 How to install a Lightmeter
- 6 Software and Installation
- 7 Lightmeter performance
- 8 Lightmeter locations
- 9 Calibration
- 10 Ideas and Requests for Improvements
- 11 Database for measurements
- 12 Conversion of light measurements
- 13 Properties of the light sensor
- 14 Note on the naming
- 15 Echo
- 16 Current Developments and Articles
This is Starlight and Lightmeter Wiki - new Version after upgrade
Important: We are recovering after and attack and things will take time for full functionality.
You can find the entire Lightmeter wiki for reading only at http://kuffner-sternwarte.at/hms
Goal: To continuously measure the state of the world's nightskies with a global network of low-cost lightmeters in the year of astronomy and to start the long-term monitoring of light pollution on Earth.
=
News
May 3rd: Mediawiki update to Version 1.22.2 completed on May 3rd; GW --NorbertHerz (Diskussion) 22:08, 3. Mai 2014 (CEST).
Sep. 26th 2013: Gabriel Stoekl (GAVO) announces the easy-Lightmeter, a Rasberry PI data logger for the Lightmeter that automaticall records and transfers data to the GAVO-database, http://licht.sternhell.at/ - the software should be released in a couple of months. GS Video: https://www.youtube.com/watch?v=kMdLVWrSRZ8 .
June 11th 2013: Report on one year of monitoring with the Vienna Lightmeter Network Licht über Wien II: Wiener Lichtbericht 2012 online at the Wiener Umweltanwaltschaft (Vienna Environmental Protection Agency).
Jan. 12th 2013: First results from the new SETAGAYA (Tokyo) station as presented at a star party on 11 Jan. at the Setagaya Planetarium. From June to December 2012 the light at night 8 km from the centre of Tokyo scatters around the maximum full-moon values but some hours during the year are 15 times darker than the full moon - still about 10 times abouve natural light at night. --GuentherWuchterl 17:03, 14. Jan. 2013 (UTC)
Be shure to check this page, to get the latest tips on running your lightmeter. Beware of the Mark 2.3 Temperature-Bug, and for problems with linux installations contact lightmeter@astronomy2009.at.
Also please upload your data to gavo [...]
Description of the Lightmeter
The lightmeter can measure all natural sky-brightnesses. It measures from starshine to sunshine.
Lightmeter performance and calibraton in the Atacama, Müller,Wuchterl and Sarazin 2011, Rev. Mex. Astrom. Astrophys. Vol. 41, pp. 46-49, , preprint(pdf),
Lightmeter technical specifications (new pdf)
Talk on the lightmeter by André Müller at the 2008 European dark sky symposium in Vienna: Low cost luxmeter (pdf,1,7MB)
How to get a Lightmeter
To get a Lightmeter download the Lightmeter request forms, fill in the data and mail it to lightmeter@astronomy2009.at
The cost of a Lightmeter is 100.- € incl. VAT.
Note that this is valid only for participants of the Lightmeter-network campaign of the Verein Kuffner-Sternwarte that makes this possible by volunteer contributions and donations.
Hardware
MarkPro 2.4
- linear domain to higher values to include the Moon and city light-levels in the linear domain
- lower noise electronics than IYA
- solar-cell in Aluminium frame with closed electronics.
- sensor made for outdoor, all-weather use; no protective housing needed
- measures: 15 x 92 x 92 mm
- mass: 370 g (270 g sensor + 100g USB-cable)
- USB-plug (needs weather protection)
- Windows support: [MarkPro 2.4 at k2wlights|http://www.k2wlights.de/indexS.html]
Mark 2.3l
- linear domain to higher values to include the Moon in the linear domain.
- low noise electronics than IYA
- solar-cell in Aluminium frame with closed electronics.
- sensor made for outdoor, all-weather use; no protective housing needed
- measures: 15 x 92 x 92 mm
- mass: 370 g (270 g sensor + 100g USB-cable)
- USB-plug (needs weather protection)
- Linux only - software: see the driver section on this wiki.
Mark 2.3 IYA - International Year of Astronome series
With the extra linear "daylight" Lux-oriented eye. This additional two channel sensor assists in calibrating the non-linear daylight range of the instrument and can be used to directly compare to Lux values as it is manufacturer calibrated and its output can be directly converted to illumination (see the driver section).
- solar-cell in Aluminium frame with closed electronics.
- sensor made for outdoor, all-weather use; no protective housing needed
- measures: 15 x 92 x 92 mm
- mass: 370 g (270 g sensor + 100g USB-cable)
- USB-plug (needs weather protection)
- additional manufaturer-calibrated, TAOS-two-channel daylight Lux-sensor (the small hole in front edge, visible in the image)
Hardware (Mark 2 original series prototype)
- solar-cell in Aluminium frame with closed electronics.
- sensor made for outdoor, all-weather use; no protective housing needed
- measures: 15 x 92 x 92 mm
- mass: 370 g (270 g sensor + 100g USB-cable)
- USB-plug (needs weather protection)
How to install a Lightmeter
To use your lightmeter you have to put it in a place with good visibility of the sky. To extend the USB-cable we recommend a USB-Ethernet-extender. For more see Lightmeter installation.
Software and Installation
You need some software on your computer. You need to install the driver that controlls the instruments and software that stores that data and displays results. See Lightmeter-Driver for information and instructions.
Lightmeter performance
The lightmeter measures fully automatic and up to 20 times per second. Measurmeents are recorded with an adjustable rate of up to once per second and are stored in a .csv or text file with fixes column width that can be easily read with standard spreadsheet software. Nighttime measurements are done in a linear mode that can be easily converted to approximate Lux-values or received energy per unit surface, like [W/m2] that can be readily related to the energy input by the Sun. To directly measure the Sun a non-linear (approximately logarithmic) daylight range operates at brightness levels above the full moon. This allows to compare daylight and nighttime variations. Alltogether the lightmeter measures from a few 100 000 Lux to 100 mikro-Lux,thus covering 11 orders of magnitude, almost as many as the human eye.
For more details see the Lightmeter technical specifications.
Lightmeter locations
Since 2006 the prototype is running in Tautenburg and since March 2009, 30 instruments of the first prototypes (Mark 2.2) are distributed and 20 are running in various places around the world. By December 2009 about 80 Lightmeters of the Year of Astronomy series (Mark 2.3) are distributes and about 40 running. This totals more than 100 Lightmeters with about 60 continuously running around the world. See the Lightmeter List for where they are located and what they measure.
For a view glimpses on the sites please check out the Berlin-Lightmeter (german language): Berlin, Platz der Vereinten Nationen, the Yonago Lightmeter, the Lindenberg station and Cerro Paranal, Chile.
--GuentherWuchterl 13:30, 29. Dez. 2009 (UTC)
Calibration
The lightmeter puts out numbers that are basically the number of electrons that are created by the light-particles when they hit the sensor and are then counted by the electronics. To get from that number or counts to a standardised quantity like received Energy per Area (Watt/square meter or in short: W/m2) or Illumination (how much much the Sensor is illuminated) in Lux, or short lx you need a calibration that converts the counts in the standardised measurement quantity in the SI-system. The calibration is usually a factor that has to be multiplied onto the counts that your lightmeter puts out. The standard calibration values to obtain a proxy for the measurement in Lux for the linear night-mode are:
- 2E-6 or 0.000002, for the Mark 2.2 (2008) series,
- 5E-7 for the Mark 2.3 (IYA 2009) series.
--GuentherWuchterl 12:50, 14. Apr. 2010 (UTC) That means e.g. you have to multiply your counts by 0.000002 to obtain the Lux-value. See Lightmeter calibration for more about the calibration of lightmeters and how to get one for your instrument.
Ideas and Requests for Improvements
The lightmeter is a new instrument and we have tried to make measurments easy as possible but only the practical use can show what is needed to get the results in the best way. See Lightmeter improvements for suggestions made and put your own ideas there.
Database for measurements
The Thüringia state observatory and the Kuffner-observatory collect the measurements to create a worldwide database for the state and history of the worlds nightskies. See Lightmeter-database for information of how to upload your data and access that data-collection.
Conversion of light measurements
Measurement of the lightmeter can be expressed in various quantities as illumination, the energy flux received by the instrument or the corresponding brightness of the sky or astronomical quantities like the mean brightness per unit area on the sky, for example in magnitudes per square arc-seconds that the Sky Quality Meter puts out.
See Conversion of light measurements for how to obtain one quantity from another one, usually with some assumptions to be made about the state of the night-sky and properties of the contributing light-sources (stars or lamps). Quantities discussed include illuminance, sky-brightness, visual limiting magnitude. Presently the discussion is mostly in German.
Properties of the light sensor
The lightmeter uses a commercial solar cell to detect and measure the light.
The sensitivity of the lightmeter is such that all natural sky-light levels can be measured That includes day and night. Thus the lightmeter can measure the Sun as well as the light emitted from very dark pristine skies in remote locations.
The lightmeter is linear from about the brightness of the full moon (about 0.3 Lux) down to the typical 0.002 Lux of dark skies and lower.
The lowest detectable signal is estimated to be the light of a single bright star as Sirus.
The measurement range above the full moon has been added to compare the daylight variations to the nighttime variations. This part is experimental and non-linear. That means twice the counts do not correspond to twice the light. These measurments have to be processed to give physical quantities correcly.
Basically the sensor records all wavelength that the eye can see and acts light an ideal detector that is sensitive to all directions: that means if you tilt it the measurements decrease as the surface of the lightmeter projection onto the plane perpendicular to the direction from which the light is shining.
For details on angular and spectral sensitivity as well as the linearity of the solar cell see Lightmeter - instrument properties
Note on the naming
The term lightmeter is more accurate than Luxmeter for the sensor used. The CIE-definition of Lux requires a narrow passband whereas the lightmeter measures over a broad range of colours including photopic, scotopic and metabolic bands. The latter broad band use is more appropriate for astronomical and enviromental purposes. For most nightsky-measurements the quantitative difference is expected to be small and the use of Lux is of advantage for comparison purposes. See What is Light Pollution? by Jan Hollan for a discussion of light-pollution definiton and measures.
Echo
http://www.scienceblogs.de/astrodicticum-simplex/2009/04/lichtverschmutzung-selber-messen.php
http://www.scienceblogs.de/frischer-wind/2009/09/dielichtsmogsensoren-sind-da.php
Current Developments and Articles
April 17th: New Mark 2.3 Windows-XP Software for hot summer days (removes bug occurring at T > 46.7°C).
March 9th: Lightmeter reaching out for the stars on top of the 30m tower at the ESO-ELT site, Cerro Armazones.
March 6th: Lightmeter performance and calibraton in the Atacama (A. Mülller et al., preprint)
Nov. 21st: Software for the Mark2.3l post IYA lightmeter online at Lightmeter Driver section.
Oct. 26th: Lightmeter 2010: The IYA-Lightmeter will be continued at the 100.- € per piece cost. The manufacturer k2wlights agreed to continue production of the Lightmeter for the linux driver - this is the Mark 2.3l series.
To get a Mark2.3l lightmeter please mail the Lightmeter request forms to lightmeter@astronomy2009.at.
k2wlights provides Windows-support for a newly developed Mark 2.4 pro version that offers an increased linear range up to 5 Lux and is faster to allow the very quick response required e.g. for mapping purposes under streetlights at speeds above 30 km/h. Contact k2wlights for details.
>160 Lightmeters worldwide (Apr 19th, 2011).
June 18th 2010: Public Lightmeter database in collaboration with the German Astrophysical Virtual Obervatory (GAVO):
- Location: http://vo.uni-hd.de/lightweather
- List of stations that are currently connected to the database,
- Sample query - to plot data scroll down and select VOplot as format.
Please upload your data! Instructions: Lightmeter-database.
Talks and articles:
- Keep it deep, G. Wuchterl on Lightmeter and World-heritage status, talk at the CEDIC 2011, March 20th 2011, Ars Electronica Centre, Linz; http://cedic.at/
- Measuring the Night Sky Brightness with the Lightmeter Lightmeter performance and calibraton in the Atacama (A. Mülller et al., preprint), Conference of Astronomical Site Testing Date in Chile, Valparaiso, 1-3 Dec 2010, http://www.dfa.uv.cl/sitetestingdata/
- Monitoring the Sky with the IYA lightmeter network, G. Wuchterl, 10th European Symposium for the Protection of the Night Sky, 2-4 September 2010, Kaposvár, Hungary, http://www.astro-zselic.hu/symposium.html
- Monitoring Night-Sky Brightness with a Lightmeter Network, G. Wuchterl,talk at 2009 European Symposium for the protection of the night skies, Armagh, Nordirland, http://www.lightpollution2009.eu/
==============================================
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