Astronomy - Stat eof the Art - CosmologyChris Impey
Astronomy - State of the Art is a course covering the hottest topics in astronomy. In this section, the properties of the whole universe are covered, including Hubble expansion, the age and size, the big bang, and dark energy.
Astronomy - State of the Art - GalaxiesChris Impey
Astronomy - State of the Art is a course covering the hottest topics in astronomy. In this section, the properties of galaxies are discussed, including supermassive black holes and dark matter.
Astronomy - State of the Art - Life in the UniverseChris Impey
Astronomy - State of the Art is a course covering the hottest topics in astronomy. In this section, the potential for life in the universe is covered, including extreme life on Earth, the Drake equation and SETI
www.cfa.harvard.edu/seuforum/mtu/MTUsizeandscale.ppt
File Format: Microsoft Powerpoint - Quick View
Size and Scale of the Universe. Image courtesy of The Cosmic Perspective by Bennett, Donahue, Schneider, & Voit; Addison Wesley, 2002. Earth. Planet where ...
Astronomy- State of the art is a course covering the hottest topics in astronomy. In this section, the exotic end states of stars are discussed, including pulsars, neutron stars, and black holes.
Astronomy - Stat eof the Art - CosmologyChris Impey
Astronomy - State of the Art is a course covering the hottest topics in astronomy. In this section, the properties of the whole universe are covered, including Hubble expansion, the age and size, the big bang, and dark energy.
Astronomy - State of the Art - GalaxiesChris Impey
Astronomy - State of the Art is a course covering the hottest topics in astronomy. In this section, the properties of galaxies are discussed, including supermassive black holes and dark matter.
Astronomy - State of the Art - Life in the UniverseChris Impey
Astronomy - State of the Art is a course covering the hottest topics in astronomy. In this section, the potential for life in the universe is covered, including extreme life on Earth, the Drake equation and SETI
www.cfa.harvard.edu/seuforum/mtu/MTUsizeandscale.ppt
File Format: Microsoft Powerpoint - Quick View
Size and Scale of the Universe. Image courtesy of The Cosmic Perspective by Bennett, Donahue, Schneider, & Voit; Addison Wesley, 2002. Earth. Planet where ...
Astronomy- State of the art is a course covering the hottest topics in astronomy. In this section, the exotic end states of stars are discussed, including pulsars, neutron stars, and black holes.
A great Power Point from Astronomy this semester, thought I would share it. This explains the properties of light and the use of Telescopes; their related properties and attributes.
in this presentation analyzing optical telescope and type of lens then lens telescope compared newton telescope in university of sulaimani. tell me for other description.
The contents of this presentation includes the history of telescope, types of telescopes: its definition, diagrams, uses, advantages and disadvantages.
Cancer cell metabolism: special Reference to Lactate PathwayAADYARAJPANDEY1
Normal Cell Metabolism:
Cellular respiration describes the series of steps that cells use to break down sugar and other chemicals to get the energy we need to function.
Energy is stored in the bonds of glucose and when glucose is broken down, much of that energy is released.
Cell utilize energy in the form of ATP.
The first step of respiration is called glycolysis. In a series of steps, glycolysis breaks glucose into two smaller molecules - a chemical called pyruvate. A small amount of ATP is formed during this process.
Most healthy cells continue the breakdown in a second process, called the Kreb's cycle. The Kreb's cycle allows cells to “burn” the pyruvates made in glycolysis to get more ATP.
The last step in the breakdown of glucose is called oxidative phosphorylation (Ox-Phos).
It takes place in specialized cell structures called mitochondria. This process produces a large amount of ATP. Importantly, cells need oxygen to complete oxidative phosphorylation.
If a cell completes only glycolysis, only 2 molecules of ATP are made per glucose. However, if the cell completes the entire respiration process (glycolysis - Kreb's - oxidative phosphorylation), about 36 molecules of ATP are created, giving it much more energy to use.
IN CANCER CELL:
Unlike healthy cells that "burn" the entire molecule of sugar to capture a large amount of energy as ATP, cancer cells are wasteful.
Cancer cells only partially break down sugar molecules. They overuse the first step of respiration, glycolysis. They frequently do not complete the second step, oxidative phosphorylation.
This results in only 2 molecules of ATP per each glucose molecule instead of the 36 or so ATPs healthy cells gain. As a result, cancer cells need to use a lot more sugar molecules to get enough energy to survive.
Unlike healthy cells that "burn" the entire molecule of sugar to capture a large amount of energy as ATP, cancer cells are wasteful.
Cancer cells only partially break down sugar molecules. They overuse the first step of respiration, glycolysis. They frequently do not complete the second step, oxidative phosphorylation.
This results in only 2 molecules of ATP per each glucose molecule instead of the 36 or so ATPs healthy cells gain. As a result, cancer cells need to use a lot more sugar molecules to get enough energy to survive.
introduction to WARBERG PHENOMENA:
WARBURG EFFECT Usually, cancer cells are highly glycolytic (glucose addiction) and take up more glucose than do normal cells from outside.
Otto Heinrich Warburg (; 8 October 1883 – 1 August 1970) In 1931 was awarded the Nobel Prize in Physiology for his "discovery of the nature and mode of action of the respiratory enzyme.
WARNBURG EFFECT : cancer cells under aerobic (well-oxygenated) conditions to metabolize glucose to lactate (aerobic glycolysis) is known as the Warburg effect. Warburg made the observation that tumor slices consume glucose and secrete lactate at a higher rate than normal tissues.
Seminar of U.V. Spectroscopy by SAMIR PANDASAMIR PANDA
Spectroscopy is a branch of science dealing the study of interaction of electromagnetic radiation with matter.
Ultraviolet-visible spectroscopy refers to absorption spectroscopy or reflect spectroscopy in the UV-VIS spectral region.
Ultraviolet-visible spectroscopy is an analytical method that can measure the amount of light received by the analyte.
Nutraceutical market, scope and growth: Herbal drug technologyLokesh Patil
As consumer awareness of health and wellness rises, the nutraceutical market—which includes goods like functional meals, drinks, and dietary supplements that provide health advantages beyond basic nutrition—is growing significantly. As healthcare expenses rise, the population ages, and people want natural and preventative health solutions more and more, this industry is increasing quickly. Further driving market expansion are product formulation innovations and the use of cutting-edge technology for customized nutrition. With its worldwide reach, the nutraceutical industry is expected to keep growing and provide significant chances for research and investment in a number of categories, including vitamins, minerals, probiotics, and herbal supplements.
(May 29th, 2024) Advancements in Intravital Microscopy- Insights for Preclini...Scintica Instrumentation
Intravital microscopy (IVM) is a powerful tool utilized to study cellular behavior over time and space in vivo. Much of our understanding of cell biology has been accomplished using various in vitro and ex vivo methods; however, these studies do not necessarily reflect the natural dynamics of biological processes. Unlike traditional cell culture or fixed tissue imaging, IVM allows for the ultra-fast high-resolution imaging of cellular processes over time and space and were studied in its natural environment. Real-time visualization of biological processes in the context of an intact organism helps maintain physiological relevance and provide insights into the progression of disease, response to treatments or developmental processes.
In this webinar we give an overview of advanced applications of the IVM system in preclinical research. IVIM technology is a provider of all-in-one intravital microscopy systems and solutions optimized for in vivo imaging of live animal models at sub-micron resolution. The system’s unique features and user-friendly software enables researchers to probe fast dynamic biological processes such as immune cell tracking, cell-cell interaction as well as vascularization and tumor metastasis with exceptional detail. This webinar will also give an overview of IVM being utilized in drug development, offering a view into the intricate interaction between drugs/nanoparticles and tissues in vivo and allows for the evaluation of therapeutic intervention in a variety of tissues and organs. This interdisciplinary collaboration continues to drive the advancements of novel therapeutic strategies.
This pdf is about the Schizophrenia.
For more details visit on YouTube; @SELF-EXPLANATORY;
https://www.youtube.com/channel/UCAiarMZDNhe1A3Rnpr_WkzA/videos
Thanks...!
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
8. Image Formation
• The focal plane is where light from different
directions comes into focus.
• The image behind a single (convex) lens is
actually upside-down!
9. Digital cameras
detect light with
charge-coupled
devices
(CCDs).
Recording Images
• A camera focuses light like an eye and captures
the image with a detector.
• The CCD detectors in digital cameras are similar
to those used in modern telescopes.
10. • Astronomers often use computer software to
combine, sharpen, or refine images.
• This image of Saturn's
moon Enceladus has
been processed to
highlight the plume of
water ice coming from
its surface.
Image Processing
11. What have we learned?
• How do eyes and cameras work?
– Eyes use refraction to bend parallel light rays
so that they form an image.
– The image is in focus if the focal plane is at
the retina.
– Cameras focus light like your eye and record
the image with a detector.
12. 6.2 Telescopes: Giant Eyes
• Our goals for learning:
– What are the two most important
properties of a telescope?
– What are the two basic designs of
telescopes?
– What do astronomers do with telescopes?
13. What are the two most important properties
of a telescope?
1. Light-collecting area: Telescopes with a
larger collecting area can gather a greater
amount of light in a shorter time.
2. Angular resolution: Telescopes that are larger
are capable of taking images with greater
detail.
14. • A telescope's diameter tells us its light-collecting
area:
• The largest telescopes currently in use have a
diameter of about 10 meters.
A = π(d / 2)2
Light-Collecting Area
15. Thought Question
How does the collecting area of a 10-meter
telescope compare with that of a 2-meter
telescope?
a) It's 5 times greater.
b) It's 10 times greater.
c) It's 25 times greater.
16. Thought Question
How does the collecting area of a 10-meter
telescope compare with that of a 2-meter
telescope?
a) It's 5 times greater.
b) It's 10 times greater.
c) It's 25 times greater.
18. Angular Resolution
• Ultimate limit to
resolution comes
from interference
of light waves
within a telescope.
• Larger telescopes
are capable of
greater resolution
because there's
less interference.
19. Close-up of a star from the Hubble
Space Telescope
Angular Resolution
• The rings in this
image of a star
come from
interference of light
wave.
• This limit on angular
resolution is known
as the diffraction
limit.
20. What are the two basic designs of
telescopes?
• Refracting telescope: focuses light with
lenses
• Reflecting telescope: focuses light with
mirrors
24. Twin Keck telescopes on
Mauna Kea in Hawaii
Segmented 10-meter
mirror of a Keck
telescope
Pick-up
images.
Pick-up
images.
Mirrors in Reflecting Telescopes
25. What do astronomers do with telescopes?
• Imaging: taking pictures of the sky
• Spectroscopy: breaking light into spectra
• Time Monitoring: measuring how light output
varies with time
30. Time Monitoring
• A light curve represents a series of brightness
measurements made over a period of time.
31. Want to buy your own telescope?
• Buy binoculars first (e.g., 7×35)—you get much
more for the same money.
• Ignore magnification (sales pitch!).
• Notice: aperture size, optical quality, portability.
• Consumer research: Astronomy, Sky & Telescope,
Mercury, astronomy clubs
32. What have we learned?
• What are the two most important properties of a
telescope?
– Collecting area determines how much light a
telescope can gather.
– Angular resolution is the minimum angular separation
a telescope can distinguish.
• What are the two basic designs of telescopes?
– Refracting telescopes focus light with lenses.
– Reflecting telescopes focus light with mirrors.
– The vast majority of professional telescopes are
reflectors.
33. What have we learned?
• What do astronomers do with telescopes?
– Imaging
– Spectroscopy
– Time Monitoring
34. 6.3 Telescopes and the Atmosphere
• Our goals for learning:
– How does Earth's atmosphere affect
ground-based observations?
– Why do we put telescopes into space?
35. How does Earth's atmosphere affect
ground-based observations?
• The best ground-based sites for astronomical
observing are:
– calm (not too windy)
– high (less atmosphere to see through)
– dark (far from city lights)
– dry (few cloudy nights)
37. Bright star viewed with
ground-based telescope
Same star viewed with
Hubble Space Telescope
Twinkling and Turbulence
• Turbulent air flow in Earth's atmosphere distorts
our view, causing stars to appear to twinkle.
38. Without adaptive optics With adaptive optics
Adaptive Optics
• Rapidly changing the shape of a telescope's mirror
compensates for some of the effects of turbulence.
39. Summit of Mauna Kea, Hawaii
Calm, High, Dark, Dry
• The best
observing
sites are atop
remote
mountains.
41. Transmission in Atmosphere
• Only radio and visible light pass easily through
Earth's atmosphere.
• We need telescopes in space to observe other
forms.
42. What have learned?
• How does Earth's atmosphere affect ground-
based observations?
– Telescope sites are chosen to minimize the
problems of light pollution, atmospheric
turbulence, and bad weather.
• Why do we put telescopes into space?
– Forms of light other than radio and visible do
not pass through Earth's atmosphere.
– Also, much sharper images are possible
because there is no turbulence.
43. 6.4 Telescopes and Technology
• Our goals for learning:
– How can we observe invisible light?
– How can multiple telescopes work
together?
44. How can we observe invisible light?
• A standard
satellite dish is
essentially a
telescope for
observing radio
waves.
45. Radio Telescopes
• A radio
telescope is
like a giant
mirror that
reflects
radio waves
to a focus.
46. SOFIA Spitzer
Infrared and Ultraviolet Telescopes
• Infrared and ultraviolet light telescopes operate
like visible-light telescopes but need to be above
atmosphere to see all wavelengths.
48. X-Ray Telescopes
• Focusing of X-rays requires special mirrors.
• Mirrors are arranged to focus X-ray photons
through grazing bounces off the surface.
52. Very Large Array (VLA)
Insert 7e, figure 6.30 here
Interferometry
• Easiest to do with
radio telescopes
• Now possible with
infrared and
visible-light
telescopes
53. What have learned?
• How can we observe invisible light?
– Telescopes for invisible light are usually
modified versions of reflecting telescopes.
– Many of the telescopes used for observing
invisible light are in space.
• How can multiple telescopes work together?
– Linking multiple telescopes using
interferometry enables them to produce the
angular resolution of a much larger telescope.
Editor's Notes
Note that the text in the book does not mention CCDs, though figure 6.6 still makes reference to them. This should be mentioned to students.
Emphasize that at a great distance the lights would look like one light rather than two --- but we could still see them. (Students sometimes think that below a particular angular resolution we see nothing at all.)
Point students&apos; attention to the human in the middle of the Keck mirror!
Optional if you wish to discuss buying your own telescope; also point students to Special Topic box on p. 177.
