Multiwavelength Analysis of Jupiter and Nebula Images

The Multiwavelength Universe Module 7 Group Presentation

Instructions 1. For EACH of the THREE images you picked: a. Make a copy of the 2 slide templates (slides #3 and #4 in this presentation) - please do not delete or alter the templates - other students will need to copy from them as well. b. Add the image you picked to the first slide template, and a title. Make sure the image has enough resolution to look good on the full screen. You don’t have to stretch it to match the placeholder - keep it in its proper aspect ratio. c. Add your description of the image to the second slide template, following the guidelines in the instructions and rubric. d. Add the references you consulted for this research to the bottom of the second slide. -LeLel MfrLeLe to pLersonHalizLe Mfonts HanKd HarrHanNgLemLent iMf you wish° 11ust mHakLe surLe thHat you’vLe mLet Hall thLe rLequirLemLents ± usLe thLe lHaIb ruIbriJc on Kd"l to LevHaluHatLe your work° 3. Once you’ve completed your slides, review your classmates’ work and leave comments using the comment feature on google slides. You should leave at least three comments (total) for full points. Try to spread your comments over multiple slides, so that everyone gets feedback.. Your comments can be: a. Suggestions for improvement b. Questions about their image c. Things they did particularly well d. ... 4. Enjoy the beautiful slideshow your team just made!

Three Types of Light from Jupiter

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Three Types of Light from Jupiter / Christopher Anacker Description: These three images of Jupiter were captured using different light from two different telescopes. The visible and ultraviolet were taken by Hubble and the infrared was taken by the Gemini North observatory in Hawaii. The most interesting feature of these three photos, which is pointed out in the article, is the Giant Red Spot. It is still seen in the visible and ultraviolet light, but almost disappears in the infrared light. In the ultraviolet light the Giant Red Spot is darker and we can see another smaller spot more clearly. The side by side comparison of my favorite planet really changed my perspective on how light can at different wavelengths affects objects References: https://cosmoquest.org/x/dailyspace/2021/05/14/tiny-unicorn-black-hole-found-in-milky-way-is-closest-one-to-earth/

+Crab Nebula

+Crab Nebula ± Mizaiel Zambrano ,WYXUXW[OVUZY[OaU`T+" The image is of the +Crab Nebula² an expanding debris field from a star’s death in the T aurus constellation° The image has radio² infrared² optical² ultraviolet² and X±ray° The telescopes used to produce the image were the VL)A² Spitzer² 0Hubble² XMM±Newton² and the +Chandra telescopes° The most prominent feature in the image is the neon coloration°The center is a pulsar that is spinning once every "" milliseconds and shooting out beams of radio and visible light°From studying the +Crab Nebula through X±ray images we have concluded that it is more condensed because we observe the electrons near the center° 1I chose this image because the +Crab Nebula seemed the most interesting to me with the different images and colors we have gotten through different wavelengths° DWXWXWW`TUW+" ZZYZYVUYX+" WYXSZ[ZTT^RW±aUXWY [O_SSYWYX VUaUZY]\]"(#!S

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*Butterfly Nebula

*Butterfly Nebula ± Mizaiel Zambrano ,WYXUXW[OVUZY[OaU`T+" This image is of the *Butterfly Nebula² a dying star° The image was taken by the 0Hubble Space Telescope and it has a variety of optical wavelengths along with ultraviolet ° The prominent features in this image are that it looks like a butterfly° *But the dying star was once about $ times the mass of the sun and its “wings” are actually cauldrons of gas° Studying the nebula in different wavelengths has let us learn about the gas² temperature and density of the dying star° 1I chose this image because 1I love butterflies and to see something resemble it in a astronomical image was amazing° )Along with the colors° DWXWXWW`TUWYX+" ZZYZYVUYX+" WYXSZ[ZTT^RW±aUXWY [O_SSYWYX ZW[OU!*!"!Z

Zeta Ophiuchi

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Zeta Ophiuchi ± Mizaiel Zambrano ,WYXUXW[OVUZY[OaU`T+" Zeta Ophiuchi is a star that likely once had a companion° The image has X±ray and infrared wavelengths and was produced by +Chandra and Spitzer° The prominent feature in this image was the story behind it° Zeta Ophiuchi was once closer in orbit with another star before it was ejected when the star went supernova° What we’ve learned from studying these stars is that we can tell why the star is no longer in orbit of the other and what gases its produced° 1I chose this image because of the name along with its story° 1I thought the name was more unique than others° DWXWXWW`TUWYX+" ZZYZYVUYX+" UZS`TVXWS±ZSXW\[SXWV±WV[Z VUZaUZYaU #!## `_`WZYSaUVUZ

Protoplanetary Disks ! Kaedence Clementson References: https://www.google.com/imgres?imgurl=https%3A%2F%2Fupload.wikimedia.org%2Fwikipedia%2Fcommons%2F9%2F9d%2FHL_Tau_protoplanetary_disk.jpg &tbnid=GJob24b0fmX60M&vet=12ahUKEwjvmKu2kKyEAxUfOkQIHdg8ADgQMygAegQIARB1..i&imgrefurl=https%3A%2F%2Fen.wikipedia.org%2Fwiki%2FPro toplanetary_disk&docid=XRlOmD95NEEZuM&w=1800&h=1800&q=protoplanetary%20disk&ved=2ahUKEwjvmKu2kKyEAxUfOkQIHdg8ADgQMygAegQIARB1

Protoplanetary Disks ! Kaedence Clementson ° Radio Wavelengths" Reveals the overall structure of the protoplanetary disk± capturing emissions from cold gas and dust² Radio observations can also detect jets of material ejected from the young star² ° /Infrared Wavelengths" .Highlights the heated dust and gas in the protoplanetary disk± providing insights into regions where planet formation is occurring² ° Visible Wavelengths" **Displays the inner regions of the protoplanetary disk± aiding in the observation of planetary formation processes² References , **Dauphas± N²± ³ Morbidelli± &''A² ´µ¶·¸¹² -Geochemical and planetary dynamical views on the origin of ++Earth’s atmosphere and oceans² /In Elsevier eBooks ´pp² ·–º»¹² https" ¼¼doi²org¼·¶²·¶·½¼b!¾ °¶°¶ °¶!»!¾»°¾²¶·º¶·°µ

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Planetary Nebulae ! Kaedence Clementson References , https" ¼¼www²google²com¼url$%%sa%"##i³url%"##https¿º&''A¿µ,F¿µ,Fscitechdaily²com¿µ,Fastronomy°astrophysics°·¶·°planetary°nebula¿µ,F³psig%"##&''AOvVaw·»iymuµsT.H·NkwZ.H¶µ,F-Gdh³u st%"##·¾¶ ¶¸ !»»»»¶¶¶³source%"##images³cd%"##vfe³opi%"## !!¾ ¸¸!³ved%"##¶))C'((BMQjRxq,FwoT))CPjj·Z))Cgr/IQ**D,FQ&''A&''A&''A&''A&''Ad&''A&''A&''A&''A&''A'((B&''A++E

Planetary Nebulae ! Kaedence Clementson ° Visible Wavelengths" Showcases the intricate and often symmetrical shapes of planetary nebulae± which are expelled layers of gas and dust from dying stars² ° Ultraviolet Wavelengths" Reveals the hot gas ionized by the dying star± offering a closer look at the energetic processes within the nebula² ° X°ray Wavelengths" ))Captures emissions from very hot gas surrounding the dying star± providing information about high°energy phenomena in the planetary nebula² References: information@eso.org. (n.d.). 7lHanLetHary 5LeIbulHa . ESA/Hubble | ESA/Hubble. https://esahubble.org/wordbank/planetary-nebula/#:~:text=A%20planetary%20nebula%20is%20a,nothing%20to%20do%20with%20planets.

Dark Matter ! Kaedence Clementson References , https" ¼¼www²google²com¼url$%%sa%"##i³url%"##https¿º&''A¿µ,F¿µ,Fscitechdaily²com¿µ,Fastronomy°astrophysics°·¶·°planetary°nebula¿µ,F³psig%"##&''AOvVaw·»iymuµsT.H·NkwZ.H¶µ,F-Gdh³ust%"## ·¾¶ ¶¸ !»»»»¶¶¶³source%"##images³cd%"##vfe³opi%"## !!¾ ¸¸!³ved%"##¶))C'((BMQjRxq,FwoT))CPjj·Z))Cgr/IQ**D,FQ&''A&''A&''A&''A&''Ad&''A&''A&''A&''A&''A'((B&''A++E

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Dark Matter ! Kaedence Clementson °Visible Wavelengths" -Gravitational lensing of dark matter can be imaged± where the mass distribution of dark matter bends and distorts the light from background galaxies² ° Radio Wavelengths" Similar to visible wavelengths± radio observations can also be used to study the gravitational lensing effects of dark matter² ° Other Observations" While not mentioned± other methods such as studying the cosmic microwave background radiation or galaxy rotation curves also contribute to understanding dark matter² References " Dark Matter ± Dark Energy ² NASA Science ² ´n²d²¹² https" ¼¼science²nasa²gov¼universe¼dark°matter°dark°energy¼

Abell ""%5&6: Untangling a Knot of Galaxy Clusters

Abell ""%5&6: Untangling a Knot of Galaxy Clusters ± Javier Flores Description - The Image you see before this is Abell 2556, a knot of galaxy clusters. Abell 2556 is located approximately 1.3 billion light-years away from Earth in the constellation of Cancer. It’s one of many galaxy clusters cataloged by George Abell in his work on galaxy clusters in the 1950s and 1960s. The wavelength from the image that you see before is a Composite wavelength. X-ray wavelength - Radio wavelength - Reference: https://chandra.harvard. edu/photo/2023/a2256/

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Multiwavelength Universe Lab 20958 - Group 2

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