EU and Greece/Sweden/Italy/France - JAHOU

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8 Δεκ 2013 (πριν από 3 χρόνια και 6 μήνες)

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http://www.euhou.net

http://www.euhou.net



Hands
-
On Universe, Europe

Bringing frontline interactive astronomy to the classroom


8 European partners


Université Pierre et Marie Curie (France)
-

F
-
HOU Coordinator


Philekpaideftiki Etaireia (Greece)


Fondazione IDIS


Citta Della Scienza (Italy)


Centrum Fizyki Teoretycznej Polskiej Akademii Nauk (Poland)


Nucleo Interactivo de Astronomia (Portugal)


Universidad Complutense de Madrid (Spain)


Onsala Space Observatory, Chalmers University (Sweden)


Armagh Planetarium (United Kingdom)



Continuous production of new innovative pedagogical resources: users
-
friendly
software, astronomical data, exercises, multimedia supports; trans
-
disciplinary in
essence (astronomy, physics, mathematics, history, language...); available in
English and in different languages.



Pedagogical use of worldwide telescope networks operated remotely via
Internet.



New innovative observing tools (webcam system, radio
-
antenna...) to be used
directly by pupils (at no cost).



Creation of a European network of researchers and middle/high school teachers
for promotion of scientific and technological education; help to gear the
education system to research and development.



web site with a free access multilingual portal to all available resources.



Dissemination through workshops and teacher training sessions.

Overall objectives


http://www.euhou.net

Web site :

1 European site and 8 national sites (
http://www.fr.euhou.net/,

etc.)

with a
C
ontent
M
anagement
S
ystem (CMS).

Each site is composed of :

+ a public Web site


+ an internal Web site/publication interface



+ an administration interface


Hosted by the server of the project (located in the UPMC computing centre,


daily back
-
up + baies RAID)



Each partner is responsible of its national site.

European interface

National interface

We are ready to welcome new partners within the web site

Robotic Telescopes in Education

Cutting edge technology

Cross
-
curricular, contribute to key skills

Exciting and stimulating projects

Student ownership of projects

Thrill of real discovery

Real time, real science

Motivating to study science/maths/ICT/technology

Exciting

Inspiring

Educational

INO

Faulkes

LCOGT
































Observing tools :


Webcam system
Skyview


The

Polish

partner

has

designed

and

produced

a

low

cost

Webcam

system

which

allows

classrooms

to

perform

themselves

night

observations
.

A

complete

software

manual

is

available,

together

with

pedagogical

tools

for

studying,

for

instance,

the

variability

of

the

brightest

stars
.


About

20

teachers

have

received

one

in

each

country
.


Observing tools :




Onsala radio telescope


The Swedish partner has
developped in Onsala a 2.3 m
prototype radio telescope,
dedicated to real time
observations via Internet
from classrooms.

A complete manual for
observing the 21 cm
hydrogen line in the Milky
Way is available.

This radio telescope can be duplicated for 10 000


(+1000


for transportation)


Observing tools :




Jodrell Bank radio


telescope


In the frame of RADIONET/FP6
-
7

the 7 m radio telescope of Jodrell
Bank is dedicated to real time
observations via Internet from EU
-
HOU classrooms during 2 months.

A complete set of educational
material for observing the 21 cm
hydrogen line in the Milky Way
and local galaxies is available.


Pedagogical resources :



SalsaJ

software


Didactical software for image and data handling


Such A Lovely Software for Astronomy, in Java



Multi
-
platform (Windows, Linux, Mac)



Java, modularity; easily extensible to implement new fonctionnalities



Adaptation in different languages; recently in arabic; chinese in progress



Free of charge (download from the EU
-
HOU web site)



Up to date sources (derived from the free medical research tool ImageJ


developed at NIH); adapted to astronomy; friendly tool for classrooms

Developed by F
-
HOU ;
SalsaJ

v2.0 to be released by the end of 2007

SalsaJ:

a multilingual interface

Pedagogical resources :



exercises

F
-
HOU:

From the Doppler effect to extrasolar planets; distances to Cepheids

Gr
-
HOU:

The life of stars; stellar population

It
-
HOU:
How to weight a distant galaxy ?

Pl
-
HOU:

Webcam astronomy; variable stars; distances to Cepheids, etc.

Pt
-
HOU:

What is a star ?

Se
-
HOU:

Radio astronomy in the classroom; hydrogen in the Milky Way

Sp
-
HOU:

The solar system as a math laboratory

UK
-
HOU:

Voyage through space (EduSpace/ESA); Faulkes telescopes


Learning science by doing science:

to propose hands
-
on activities based on real


astronomical data, inspired from research:

GOAL

Introduce high school students to theoretical
models in physics and astronomy


Stellar model

Planck’s law

Stefan
-
Boltzmann’s
law

Wien’s law

HR Diagram

www.gr.euhou.net/





The Swedish contribution to EU
-
HOU:

A Hands
-
On Radio
Astronomy

exercise


Mapping

the Milky Way
using atomic hydrogen

Hydrogen 21 cm
line


Hydrogen

(H)


the most
abundant element in the
universe


Abundant in our Galaxy


Atomic hydrogen in the
ground state


hyperfine
transition


The electron’s spin
becomes anti
-
parallel
to the proton’s


Radiation at
1420 MHz



21 cm

is emitted


Radio frequency


the
atmospheric window

is
open


rotation
Galactic
Perseus arm
Cygnus arm
Orion arm
Sun
l=270
l=0
Quadrant I
Quadrant IV
Sagittarius arm
Centaurus arm
C
Quadrant II
Quadrant III
l=90
l=180
10 kpc = 32 600 light-years
Radio spectrum


Observations in the Galactic disc


The purple line: line
-
of
-
sight


Radio lines correspond to spiral arms

Rotation Curve


Keplarian rotation

(Solar system)


V
~1/
R


Solid body rotation

(cdrom…)


V
~
R


Differential rotation

(The Milky Way)


V
=Constant


Dark matter



Dynamical


effects


Astrometry



Radial


velocity



Timing



M
P
sin i

Circular orbit

Elliptical orbit


Time


Time

Virginis


doublet du sodium


11 spectra

Spectre

Date

t

(days)


1

( Ǻ)


1 Ǻ = 10
-
10

m

Dl =
λ
1
-

λ
Na1

( Ǻ)

1 Ǻ = 10
-
10

m

V
E

= c

.(λ
1
-

λ
Na1
)/ λ
Na1

(km/s)

1

0

5890,411

0.461

23.48

2

0.974505

5890,496

0.546

27.81

3

1.969681

5890,491

0.541

27.56

4

2.944838

5890,305

0.355

18.08

5

3.970746

5890,014

0.064

3.26

6

4.886585

5889,815

-
0.135

-
6.88

7

5.924292

4889,642

-
0.308

-
15.69

8

6.963536

5889,638

-
0.312

-
15.89

9

7.978645

5889,764

-
0.186

-
9.47

10

8.973648

5890,056

0.106

5.40

11

9.997550

5890,318

0.368

18.74

Radial velocity curve

as a function of time

V
rad

=
V
0

+
W



cos ( 2
p
t/
T

+ b)

=
5,9 (km/s)

+
23,2 (km/s) ∙

cos (
2p
t
days
/(
10,4
days
)

+ b)

w

w

V
0

T/2 = 5,2 days


Kepler law ; m<<M m sin i ≈ (P/2
π
G)
1/3
(V
rad
)M
2/3

(1


e
²
)
1/2

• The black hole at the center of the Milky Way


• Estimation of the Hubble constant

How to weight

a galaxy ?


Dl / l = 2
v
longitudinal

/ c


= 2 v sin(i) / c

To weight a galaxy










Dl / l = 2
v
longitudinal
/ c = 2 v
sin(i) / c


l
2
 l


= 22 pixels ≈ 20 Å

Dl = 
pixels

2 r = 20 pixels

M ≈ 10
40

kg

0,82
arcsecs

39,7 Mpc

1 pixel

Vitesse de rotation des bras autour du noyau de la galaxie

:

Le décalage spectral augmente à partir du noyau pour atteindre une valeur quasi constante v
7

de 7 pixels lorsque la
distance au centre du noyau dépasse 10 pixels.

V
7

= (7/7231). 3 .10
8

/ (2 sin(53
°
)) = 181 km/s

Distribution de masse

et rayon d’action

:

Nous supposons une distribution homogène à symétrie sphérique, nous prenons r = 10 pixels (
c’est notamment ce point
que l’on peut discuter et que la version approfondie de l’exercice permettra d’améliorer
).

D’autre part, la galaxie est à 39,7 Mpc de distance




0,82 arcsecs/pixels

; 1 arcsec =
p
/ (180.60.60) = 4,85. 10
-
6

rad

; 1pc = 3,09. 10
16

m ,


d’où 1 pixel = angle en radian . distance en mètres


1 pixel = 0,82. 4,85 . 10
-
6
. 3,09. 10
16

. 39,7.10
6

m = 4,88.10
18

m

Estimation «

mécanique

» de la masse pour r ≈ 10 pixels


M = v² r / G = ( 1,81.10
5


. 4,88. 10
19

/ 6,67 . 10
-
11


M = [1,81².4,88/6,67] . 10
40

kg ≈ 10
40

kg


Ceci est bien l’ordre de grandeur des masses des galaxies

; la masse effective de la galaxie sera d’autant plus grande
qu’on étendra r

; pour des calculs plus fins, voir la version approfondie de cet exercice.


Dissemination :



Leaflets



Web site



Stages for students



TRA training sessions



Events

«

Human

» solar system or
Orrery





Stages L3/UPMC at the Armagh Observatory
(in English)


Kepler laws


Bethleem star

Then, students can visit schools in France

Dissemination :

teacher training

Training workshops in
E
nglish were
proposed to TRA (cost covered):

almost
100 teachers

Torun (Poland) 20
-
23 October 2005;

OHP 9
-
12 March 2006;

Napoli 21
-
24 September 2006.

Plus national training.

Training Resource Agents

(TRA)


are teachers eager to :



learn about the various EU
-
HOU outputs



adapt European resources to national curricula



use them in their schools



train other teachers/educators about the


resources





Thank you