05_a_the_microscope.ppt
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This document discusses microscopes and their parts and functions. It begins by defining a microscope as an optical instrument used to magnify very small objects so their structure can be examined. It then describes the basic parts of light microscopes, including their optical parts like objectives and oculars, and mechanical parts like the stage and focus knobs. Examples of specimens viewed under different magnifications are provided, such as protozoans and paramecium. Formulas for calculating total magnification are given based on the eyepiece and objective magnifications. The document concludes with sample microscope questions about magnification levels and lens combinations.
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Microscopy involves using microscopes or microscope objectives to obtain greater detail of small samples or objects. A microscope uses a combination of lenses to produce highly magnified images. Key components include the objective lens closest to the sample, the eyepiece lens closest to the observer, and a light source. Magnification is the ratio of the size of an object seen under the microscope compared to its actual size. Resolution is the ability to differentiate between two close points. Common types include compound microscopes, which use multiple lenses to magnify images, and electron microscopes, which use electron beams.
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The document provides information about microscopy, including:
1. Defining key microscope terms like magnification, resolving power, contrast, and depth of field.
2. Describing the parts and proper use of compound light microscopes, including objectives, oculars, stages, condensers, and focusing.
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2) A brief history highlighting early pioneers like van Leeuwenhoek who made important early discoveries.
3) Descriptions of common microscope types like compound, phase contrast, and electron microscopes.
4) Explanations of key microscope components like the objective lens, eyepiece, stage, and illumination methods.
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1. It defines microscopy as using an instrument called a microscope to view objects too small to see with the naked eye.
2. It describes some key parts and types of microscopes like compound, phase contrast, dark ground, and electron microscopes.
3. It explains concepts like magnification, resolution, and aberration that are important for microscopy.
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Microscope
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History
Compound microscope
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Dark field microscope
Phase contrast microscope
Fluorescent microscope
Polarising microscope
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A Microscope is an instrument for viewing objects that are too small to be seen by the naked/ unaided eyes.
In Greek micron= small
skopien=to look at
The science of investigating small object using such an instrument is called microscopy
The term microscopic means minute or very small, not visible with the eye unless aided by a microscope
From ancient times, man wanted to see things for smaller than could be perceived with the naked eye.
This led to the construction in the 16th century, of a magnifier composed of a single convex lens, and this in turn led to the eventual development of the microscope.
The most famous early pioneers in the history of microscope are Digges of England and Hans & Zcharias Janssen of Holland
It was Antony Van Leeuwenhoek who became the man to make and use a real microscope.
Leeuwenhoek microscope was called as single lens microscope because it had convex lens attached to metal holder and was focused using screws
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This document provides instructions on how to use a compound light microscope. It describes the main parts of the microscope, including the eyepiece, objectives, stage, focus knobs, light source, frame, and base. It explains that total magnification is calculated by multiplying the objective and ocular magnifications. The document also outlines general procedures for carrying, setting up, focusing, and storing the microscope safely. Key steps include using the coarse focus to initially view the specimen, fine focusing for clarity, switching objectives while re-focusing, and adjusting the light as needed.
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This document provides an overview of microscopes, including their history, types, parts, functions, and proper use and care. It discusses the earliest simple microscopes in the 16th century and key developments like the compound microscope in the 17th century. The main types covered are the compound light microscope, electron microscopes like the SEM and TEM, and dissection microscopes. The parts of a typical compound microscope and their functions are defined. Proper focusing techniques and use of oil immersion objectives are also outlined.
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The document discusses different types of microscopes and their parts and uses. It describes the history of the microscope from its invention in the 1590s. It explains that a compound microscope uses multiple lenses to magnify specimens, while a stereo microscope is used for dissection. The key parts of a microscope are identified like the objective lenses, stage, light source, and ocular lens. It provides instructions on how to properly use a microscope, focusing first on low magnification and using the fine adjustment knob to sharpen the image.
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2. An optical microscope uses lenses and light to magnify small samples. It has various parts like the stage, eyepieces, objective lenses, and rack and pinion mechanisms.
3. The experiment involved identifying each part's function, understanding the microscope's working mechanisms, and then reassembling the microscope.
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The document describes the main parts of a microscope and their functions. It explains that a microscope uses lenses to magnify small objects. The main parts include the arm, base, eyepiece, body tube, revolving nosepiece, stage, objective lenses, fine and coarse adjustment knobs, slide holder, diaphragm, light source, and on/off switch. It also provides instructions for properly focusing a microscope and handling/storing the device.
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The Milky Way’s (MW) inner stellar halo contains an [Fe/H]-rich component with highly eccentric orbits, often referred to as the
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because the morphology of debris depends on how long it has had to phase mix. The recently identified phase-space folds in Gaia
DR3 have positive caustic velocities, making them fundamentally different than the phase-mixed chevrons found in simulations
at late times. Roughly 20 per cent of the stars in the prograde local stellar halo are associated with the observed caustics. Based
on a simple phase-mixing model, the observed number of caustics are consistent with a merger that occurred 1–2 Gyr ago.
We also compare the observed phase-space distribution to FIRE-2 Latte simulations of GSE-like mergers, using a quantitative
measurement of phase mixing (2D causticality). The observed local phase-space distribution best matches the simulated data
1–2 Gyr after collision, and certainly not later than 3 Gyr. This is further evidence that the progenitor of the ‘last major merger’
did not collide with the MW proto-disc at early times, as is thought for the GSE, but instead collided with the MW disc within
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•Post-harvestlossesaccountforabout10%oftotalfoodgrainsduetounscientificstorage,insects,rodents,micro-organismsetc.,
•Totalfoodgrainproductioninindiais311milliontonnesandstorageis145mt.InIndia,annualstoragelosseshavebeenestimated14mtworthofRs.7,000croreinwhichinsectsaloneaccountfornearlyRs.1,300crores.
•InIndiaoutofthetotalproduction,about30%ismarketablesurplus
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A Microscope is an instrument for viewing objects that are too small to be seen by the naked/ unaided eyes.
In Greek micron= small
skopien=to look at
The science of investigating small object using such an instrument is called microscopy
The term microscopic means minute or very small, not visible with the eye unless aided by a microscope
From ancient times, man wanted to see things for smaller than could be perceived with the naked eye.
This led to the construction in the 16th century, of a magnifier composed of a single convex lens, and this in turn led to the eventual development of the microscope.
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- Organisms can be either unicellular or multicellular. Populations are groups of the same species in an area. Communities include all species in an area. Ecosystems include all communities and physical components in an area.
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The document describes the main parts of a microscope and their functions. It explains that a microscope uses lenses to magnify small objects. The main parts include the arm, base, eyepiece, body tube, revolving nosepiece, stage, objective lenses, fine and coarse adjustment knobs, slide holder, diaphragm, light source, and on/off switch. It also provides instructions for properly focusing a microscope and handling/storing the device.
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The Milky Way’s (MW) inner stellar halo contains an [Fe/H]-rich component with highly eccentric orbits, often referred to as the
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collided with the MW proto-disc 8–11 Gyr ago, and the Virgo Radial Merger (VRM), where the progenitor collided with the
MW disc within the last 3 Gyr. These two scenarios make different predictions about observable structure in local phase space,
because the morphology of debris depends on how long it has had to phase mix. The recently identified phase-space folds in Gaia
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at late times. Roughly 20 per cent of the stars in the prograde local stellar halo are associated with the observed caustics. Based
on a simple phase-mixing model, the observed number of caustics are consistent with a merger that occurred 1–2 Gyr ago.
We also compare the observed phase-space distribution to FIRE-2 Latte simulations of GSE-like mergers, using a quantitative
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were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
The binding of cosmological structures by massless topological defects
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
Anti-Universe And Emergent Gravity and the Dark Universe
Recent theoretical progress indicates that spacetime and gravity emerge together from the entanglement structure of an underlying microscopic theory. These ideas are best understood in Anti-de Sitter space, where they rely on the area law for entanglement entropy. The extension to de Sitter space requires taking into account the entropy and temperature associated with the cosmological horizon. Using insights from string theory, black hole physics and quantum information theory we argue that the positive dark energy leads to a thermal volume law contribution to the entropy that overtakes the area law precisely at the cosmological horizon. Due to the competition between area and volume law entanglement the microscopic de Sitter states do not thermalise at sub-Hubble scales: they exhibit memory effects in the form of an entropy displacement caused by matter. The emergent laws of gravity contain an additional ‘dark’ gravitational force describing the ‘elastic’ response due to the entropy displacement. We derive an estimate of the strength of this extra force in terms of the baryonic mass, Newton’s constant and the Hubble acceleration scale a0 = cH0, and provide evidence for the fact that this additional ‘dark gravity force’ explains the observed phenomena in galaxies and clusters currently attributed to dark matter.
ESA/ACT Science Coffee: Diego Blas - Gravitational wave detection with orbita...
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Presentation in the Science Coffee of the Advanced Concepts Team of the European Space Agency on the 07.06.2024.
Speaker: Diego Blas (IFAE/ICREA)
Title: Gravitational wave detection with orbital motion of Moon and artificial
Abstract:
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We present the JWST discovery of SN 2023adsy, a transient object located in a host galaxy JADES-GS
+
53.13485
−
27.82088
with a host spectroscopic redshift of
2.903
±
0.007
. The transient was identified in deep James Webb Space Telescope (JWST)/NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) program. Photometric and spectroscopic followup with NIRCam and NIRSpec, respectively, confirm the redshift and yield UV-NIR light-curve, NIR color, and spectroscopic information all consistent with a Type Ia classification. Despite its classification as a likely SN Ia, SN 2023adsy is both fairly red (
�
(
�
−
�
)
∼
0.9
) despite a host galaxy with low-extinction and has a high Ca II velocity (
19
,
000
±
2
,
000
km/s) compared to the general population of SNe Ia. While these characteristics are consistent with some Ca-rich SNe Ia, particularly SN 2016hnk, SN 2023adsy is intrinsically brighter than the low-
�
Ca-rich population. Although such an object is too red for any low-
�
cosmological sample, we apply a fiducial standardization approach to SN 2023adsy and find that the SN 2023adsy luminosity distance measurement is in excellent agreement (
≲
1
�
) with
Λ
CDM. Therefore unlike low-
�
Ca-rich SNe Ia, SN 2023adsy is standardizable and gives no indication that SN Ia standardized luminosities change significantly with redshift. A larger sample of distant SNe Ia is required to determine if SN Ia population characteristics at high-
�
truly diverge from their low-
�
counterparts, and to confirm that standardized luminosities nevertheless remain constant with redshift.
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Themajorcausesofdeteriorationinstorage
•Physical
•Biological
•Mechanical
•Chemical
Storageonlypreservesquality.Itneverimprovesquality.
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Classification
Metal ion ion indicators
Masking and demasking reagents
Estimation of Magnisium sulphate
Calcium gluconate
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1.Direct Titration
2.Back Titration
3.Replacement Titration
4.Indirect Titration
Masking agent, Demasking agents
formation of complex
comparition between masking and demasking agents,
Indicators/Metal ion indicators/ Metallochromic indicators/pM indicators,
Visual Technique,PM indicators (metallochromic), Indicators of pH, Redox Indicators
Instrumental Techniques-Photometry
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Miscellaneous methods.
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Wellprovedthatnogranariescanbefilledwithgrainswithoutinsectsastheharvestedproducecontainegg(or)larvae(or)pupae(or)adultinsectinthembecauseoffieldcarryoverinfestationwhichcannotbeavoidedindevelopingcountrieslikeIndia
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Graininfestation
Directdamage
Indirectly
•theexuviae,skin,deadinsects
•theirexcretawhichmakefoodunfitforhumanconsumption
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05_a_the_microscope.ppt
- 2. MICRO = SMALL SCOPE = TO VIEW MICROSCOPE: “an optical instrument consisting of a lens or combination of lenses, which magnify very small objects so that their structure or texture may be examined.”
- 3. • Microscopes are made up of various parts that work together to give a magnified view of an object.
- 4. • Simple microscope – single convex lens (“magnifying glass”). Magnifies the object.
- 5. • Compound microscope – objective lens and eyepiece lens. Gives greater magnification. (Magnifications of lenses are multiplied.)
- 6. PARTS OF THE LIGHT MICROSCOPE Optical Parts
- 7. POWER CORD 8. LAMP 7. DIAPHRAGM 5. HIGH- POWER OBJECTIVE 9. OCULAR (EYEPIECE) 1. Body tube
- 8. PART: FUNCTION: Body tube Supports the eyepiece Diaphragm Controls light intensity (brightness) Objective lens Magnifies object Ocular Magnifies image
- 9. PARTS OF THE LIGHT MICROSCOPE Mechanical Parts
- 10. 14. BASE 10. ARM 6. STAGE & STAGE CLIPS 12. COARSE ADJUSTMENT (FOCUS) KNOB 13. FINE ADJUSTMENT (FOCUS) KNOB
- 11. PART: FUNCTION: Base Supports the microscope Arm Supports lenses Stage Supports object Coarse adjustment Gets image into approximate focus Fine adjustment Gets image into exact focus
- 12. THE VIEW THROUGH THE EYEPIECE SCABIES MITE
- 13. BIOPOLYMER MESH
- 14. Protozoan (60 x)
- 16. Vorticella
- 18. Magnification • The compound light microscope can be used to view specimens that have dimensions smaller than 0.1 mm. • You can calculate the total magnification of a specimen by multiplying the magnification of the eyepiece lens by the objective lens. • For example: – 10x X 4x = 40x total magnification – (eyepiece) X (objective) = total magnification
- 19. Magnification continued • The greater the total magnification, the smaller the field of view (FOV). The lower the total magnification, the larger the FOV. • Most microscopes have a 10x eyepiece and three objective lenses of different magnifications. – 4x objective for scanning the slide – 10x objective – low power – 40x objective – high power (only use fine adjustment knob with this lens)
- 20. Answer questions 1-3 on Microscopic Proportions entry 1 Calculate the total magnification: a. 15x X 15x = 225x b. 10x X 10x = 100x c. 20x X 40x = 800x 2. With which combination of lenses would you be able to see the largest area of a specimen? 10x eyepiece & 4x scanning. The smallest? 10x eyepiece & 40x high power. 3. Which set of lenses would you use to locate a speciment on a slide? Scanning objective (4x). Which set would you use to examine the details of the specimen? High power objective (40x).