Light Pollution Measured by the DSS-7 (Deep Space Spectrograph)Rose Haberhttp://farm1.static.flickr.com/61/212916043_7895484234.jpgChicago, Illinois at night

NeedGlareLight TrespassHarms wildlife Wastes government money-Cinzano, 2009

Vancouverhttp://farm1.static.flickr.com/101/285102672_4203221326.jpg

http://www.noaanews.noaa.gov/nightlights/blackout081403-20hrsbefore-text.jpg

Light PollutionMisdirected or misused lightInappropriate application of exterior lighting productsLight causing a glow over urban/suburban areashttp://farm2.static.flickr.com/1293/554194288_965f5494cb.jpg

Spectroscopy Spectrograph- takes light from a source and separates it by wavelengthhttp://loke.as.arizona.edu/~ckulesa/camp/spectroscopy_intro.html

Stellar Spectroscopyhttp://cass.ucsd.edu/public/tutorial/Stars.html

Spectrograph Fundamentalshttp://imgsrc.hubblesite.org/hu/db/images/hs-2002-10-c-web.jpg

http://www.sbig.com/dss7/dss7.htmThe DSS-7Absorption lines for different chemicalshttp://imgsrc.hubblesite.org/hu/db/images/hs-2002-10-c-web.jpg

CCD ImagingST-7XME CCD Camerahttp://www.sbig.com/sbwhtmls/online.htmhttp://imgsrc.hubblesite.org/hu/db/images/hs-2002-10-c-web.jpg

Maxim DLPhoto-Processing image stacking software

Spectrum of the night sky at Mound Ekar Observatory Natural sky lines/ artificial lightinghttp://adsabs.harvard.edu/full/2000MmSAI..71..235R

Literature ReviewProposal of a Spectroscopic Map of Astronomical SitesRosoni, 1997

Literature Review ContinuedModeling of Light Pollution in Suburban Areas Using Remotely Sensed Imagery and GIS Chalkias et. al, 2006http://geoinformatics.sut.ac.th/sut/student/GISpresent/2006-1/light.pdf

Literature Review ContinuedCoupling MOAO with Integral Field Spectroscopy: specifications for the VLT and the E-ELTPuech et al., 2002http://arxiv.org/pdf/0808.1196v1

http://www.cfai.dur.ac.uk/new/spectroscopy/ifu_tech_s.jpg

Literature Review ContinuedVisual measurements and spectral survey of night sky brightness in Venezuela and ItalyF. Della Prugna, 1999http://aas.aanda.org/index.php?option=article&access=doi&doi=10.1051/aas:1999426

Purposehttp://imgsrc.hubblesite.org/hu/db/images/hs-2002-10-c-web.jpgTo examine the difference between the pollution of light in Manhasset, NY as opposed to the lack of pollution in Montauk, NY.

HypothesisNull Hypothesis: no difference between the light pollution in both areasAlternate Hypothesis: light pollution will be greater in Manhasset than in Montauk

http://imgsrc.hubblesite.org/hu/db/images/hs-2002-10-c-web.jpg

MethodologyLight Pollution Measured by the DSS-7 Control: sky measured by DSS-7 in Montauk, NYVariable: sky measured DSS-7 in Manhasset, NYProcedureSpectrograph attached to the CCD imager, many images taken to examine types of light pollutants, images processed and stacked using Maxim DL softwareMeasurementMeasured once a week in Montauk and imaged, measured once a week in Manhasset and imaged over 7 monthsAnalysisGraph/map of data collectedAmounts vs. types of light pollution analyzedhttp://imgsrc.hubblesite.org/hu/db/images/hs-2002-10-c-web.jpg

Study done in accessible placesManhasset, NYMontauk, NY/ Upstate, NYCCD imager/DSS-7 easily portableSoftware downloaded for free off SBIG website/astronomy coolwikiDo-Abilityhttp://imgsrc.hubblesite.org/hu/db/images/hs-2002-10-c-web.jpg

Budgethttp://imgsrc.hubblesite.org/hu/db/images/hs-2002-10-c-web.jpg

Sheet1

Item NameVendorItem #QuantityDescriptionPriceTotal Price

DSS-7SBIGDSS-71Deep space spectrograph (optimized for ST-402ME and f/10 SCT scopes)$1,595$1,595

ST-7XME CCD CameraSBIGST-7XME Std1Dual sensor, USB camera with KAF-0402ME Class 2 CCD, Remote Guide Head Port, Water Cooling Ready$2,195$2,195

TOTAL$3,790

Sheet2

Sheet3

Works Cited

Chalkias, C., M. Petrakis, B. Psiloglou, and M. Lianou. "Modelling of light pollution in suburban areas using remotely sensed imagery and GIS." Journal of Environmental Management 76 (2004)): 57-63. Elesiver. Department of Geography, Harokopio University, 19 Sept. 2005. Web. http://geoinformatics.sut.ac.th/sut/student/GISpresent/2006-1/light.pdfCinzano. "Light Pollution Information by Starry Night Lights." Night Sky Friendly Outdoor Lighting. N.p., 2009. Web. http://www.starrynightlights.com/lpIndex.htmlCole, Gary M. "A Pellicle Autoguider for the DSS-7 Spectrograph." Pellicle Autoguider (2006): 153-56. Pellicle Autoguider. Starphysics Observatory, 2007. Web. http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?2007SASS...26..153C&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdfHolmes, Alan. "DSS-7 Deep Space Spectrograph." SBIG Santa Barbara Instrument Group. N.p., 20 Mar. 2002. Web. http://www.sbig.com/dss7/dss7.htmKaler, James. "Obtaining Astronomical Spectra- Spectrographs." Australia Telescope Outreach and Education. CSIRO Australia, 23 June 2004. Web. http://outreach.atnf.csiro.au/education/senior/astrophysics/spectrographs.htmlKulesa, Craig. "What is Spectroscopy?" What is Spectroscopy? N.p., 4 Feb. 1997. Web. http://loke.as.arizona.edu/~ckulesa/camp/spectroscopy_intro.htmlLa Pointe, Robert. "Measuring the Hubble Constant Using SBIG's DSS-7." NASA Astrophysics Data System (2008): 137-40. Society for Astronomical Sciences Inc., 2008. Web. http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?2008SASS...27..137L&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdfLicker, Mark D. Dictionary of Astronomy page 101; 2003 Plavec, Mirek J.; Stellar Evolution McGraw-Hill,1997, pp 392-401. Prugna, F. Della. "Visual measurements and spectral survey of night sky brightness in Venezuela and Italy." The European Southern Observatory (n.d.): n. pag. Astronomy and Astrophysics. Centro de Investigaciones de Astronom CIDA, 9 Sept. 1999. Web. http://aas.aanda.org/index.php?option=article&access=doi&doi=10.1051/aas:1999426Puech, Michael, H. Flores, Michael Lehnert, B. Neichel, T. Fusco, P. Rosati, J.-G. Cuby, and Gary Rousset. "Coupling MOAO with Integral Field Spectroscopy: specications for the VLT and the E-ELT." Observatoire de Paris (n.d.): n. pag. LESIA. Laboratoire dstrophysique de Marseille, 8 Aug. 2008. Web. http://arxiv.org/pdf/0808.1196v1Reviglio, Pietro M., and David J. Helfand. "Active Galaxies in the Sloan Digital Sky Survey I: The Spectroscopically Unremarkable Population of the Local Universe." (2008): n. pag. Astronomy Department. Astronomy Department, Columbia University, 2008. Web. http://arxiv.org/pdf/0902.1766v1Richmond, Michael. "Spectrographs and Spectra." Spectrographs and Spectra. N.p., n.d. Web. http://spiff.rit.edu/classes/phys301/lectures/spectra/spectra.htmlRosoni, Stefano. "Proposal of a spectroscopic map of astronomical sites." Memorie della Societa Astronomia Italianap.235 71 (1997): 235-38. Circolo Astronomico Dorico. Paolo Andrenelli, 1997. Web. http://articles.adsabs.harvard.edu/full/2000MmSAI..71..235RSmith, Gene. "Stellar Spectra." Center for Astrophysics & Space Sciences, UCSD. N.p., 16 Apr. 1999. Web. .

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glare:light shining dangerously out into peoples eyes as they walk or drive by.Light Trespass: unwanted light shining onto a neighbors property or into their home.Light Pollution Wastes- billions of dollars annually in the United States. 5 to 10 billion depending on whose numbers you want to use.Light Pollution Harms: nocturnal wildlife. Many species won't even go near an area that has bad lighting. Also, many species will simply stop reproducing if habitat destruction from overly bright lights becomes too severe. Light Pollution currently threatens all Florida Sea Turtles.

Light pollution is essentially misdirected or misused lightResults from inappropriate application of exterior lighting productsLight wastefully escaping into the night sky and causing a glow over urban/suburban areas.a spectrograph is a device that can produce a graph of the intensity of light as a function of color, or wavelength. A spectrometer is a device that measures only one selectable color, and a monochromator is a device that transmits only one color. The DSS-7 spectrograph is designed to separate and focus wavelengths from 4000 to 8000 angstroms across the width of an ST-7 CCD. The human eye is sensitive from about 4500 (deep blue) to 7000 (deep red) angstroms, with its peak sensitivity at 5550 angstroms. The silicon CCDs used in SBIGs cameras have a larger range of sensitivity than the eye. Most stars put out a continuum of wavelengths with a number of absorption lines superimposed on it. Most emission nebula like the Orion Nebula produce a spectrum this is composed of a few bright emission lines, such as H-alpha (a hydrogen line at 6563 angstroms), H-beta (a hydrogen line at 4861 angstroms), and O-III (a triply ionized oxygen line at 5007 angstroms). An angstrom is one ten billionth of a meter. You will also quite often see wavelengths written in nanometers, which is one billionth of a meter. 6563 angstroms (A) is 656.3 nanometers (nm). Galaxies have a spectrum that is an aggregate of many stars, and have a similar spectrum. Most galaxies only have a few obvious features the cores tend to show a sodium absorption line due to the older stars there. Seyfert galaxies and other active galaxies show an excess of H-alpha, which is great since it makes a red shift much easier to determine. Quasars, nova and supernova in general exhibit strong 6563 emission. In the case of quasars it can be red shifted quite a bit, hundreds of angstroms, so it may actually appear at a different wavelength. For a nova, the line will only be shifted slightly since the star is in our own galaxy, but it may be greatly broadened. The individual hydrogen atoms are moving very fast due to the tremendous temperatures involved, producing Doppler broadening that smears out the line.SBIGs new Deep Space Spectrograph (DSS-7) is a spectrograph optimized for the types of spectral observations that an amateur has always been interested in, from stellar classification to nebular analysis to galactic red shifts.Light enters the spectrograph through an entrance slit and is folded and then collimated (made parallel) by the collimation lens. The light then impinges upon a diffraction grating, which causes different colors to be reflected at different angles.Stars can be classified spectrally into the well know OBAFGKM groups. The very hot stars have few features in their spectrum, perhaps only a few hydrogen lines. The spectrum of Vega shown later illustrates this. The cool stars tend to be old, with many metallic lines producing a very complex and structured spectrum. There are also several types of peculiar stars, which show strong emission lines or other structure. The DSS-7 can reveal these features.The DSS-7 is designed to accept an F/10 cone of light, a value typical of popular commercial Schmidt-Cassegrain telescopes. In the imaging mode, it acts like a 2:1 focal reducer, increasing the field of view of the CCD. It also is effectively a 2:1 focal reducer in spectrograph mode, increasing the sensitivity to extended objects like nebulas or galaxies. It will accept the center portion of the cone of light from a faster telescope, but light is lost around the edges of the collimator lens.The small DC motors in the DSS-7 are powered by a 9 volt battery. The motors are controlled by signals from the CCD camera relay port through a phone jack connector. There is no provision for guiding. Knowledge of spectroscopal map- allows for better study of propagation of light pollution Rosoni, 1997