Application for the Post of Ph.D. at Star and Planet Formation Group, Institute for Astronomy ETH Zurich

A. Identification:

Name DHAIRYASHIL HANAMANTRAO JAGADALEFirst Middle Last (Family Name)

Current: 5, Shivdarshan Appt. Permanent: A/P: Budh,Address Visava Park, Address Tal: Khatav, Dist: Satara, Pirwadi, Dist: Satara (MAharashtra), Satara (Maharashtra), India: 415503 India: 415003

Telephone +91 9421213195 Telephone +91 9561583195

FAX - e-mail dhjagadale@gmail.com

Do you require financial aid? YES (If “no”, please attach a statement describing your means of support.)

B. Personal data:

Date of birth 07/ 15/ 1986 Place of Birth: Budh (MH), India (mo.) (day) (yr.)

Married NOT MARRIED,

Citizenship INDIAN

Optional question: Gender: Male YES

TOEFL Scores: Appearing.

Place : PUNE (INDIA) Date : 30/11/2009

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CURRICULUM VITAEDhairyashil H. Jagadale

dhjagadale@gmail.comCell: +91 9421213195

I think to: Work reliably with heartily involvement to understand the fundamental laws of physics.

Research Activities:

M.Sc. Project:

I. “Study of Star Formation Rate in Spiral Galaxy NGC6951”, (Aug 2007- April 2008), under Supervision of Prof. Swara Ravindranath, IUCAA, Pune (India) and Prof. R. K. Dabhade, Fergusson College, Pune.

II. “A Study of Star Formation in Starburst Galaxies”, (May 2008-Feb. 2009), under Supervision of Prof. Swara Ravindranath, IUCAA, Pune (India) and Prof. R. K. Dabhade, Fergusson College, Pune.

III. “Massive GWs and Their Signature on CMB Polarization Spectrum” (April 2009- Oct.2009), self guided project, Discussion with IUCAA scientists.

IV. “Black Hole Entropy as a Perceiver of Quantum Gravity”, (May 2009- ), self guided project, Discussion with IUCAA (www.iucaa.ernet.in ) scientists.

B.Sc. Projects:

I. “Cosmology: Comparative Study of Cosmological Theories and Aspects of Modern Cosmology” (July 2005 - Dec 2005) under supervision of Dr. L. D. Kadam, YCIS (http://www.erayat.org/ycis/ ), Satara (India), (Received first prize).

II. “A Photometric Study of Globular Clusters”, (July 2005 - Dec 2005) under supervision of Dr. L. D. Kadam, YCIS (http://www.erayat.org/ycis/ ), Satara (India).

Publications:1. Presented and published a poster “Star Formation Rate in Spiral Galaxies as a Function of

Galactic Properties” organized by Modern College, Pune and Indian Physics Association (Pune Chapter), March 2008.

2. Successively observed the meteor shower “Geminids” and published to IMO, December 2004, 2005, 2006.

3. “Methods of Building Newtonian telescope ” organized by Ranawata, Satara, at Satara, August 2005.

4. Edited a text book named “A Guide of Astronomy” at YCIS, Satara, February 2005.

Publications in Pipeline:1. Co-author of the book “Introduction to Astronomy and Astrophysics” for amateur

Astronomers, January 2009 - onwards.

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2. “The classical to quantum transition of moments of inertia of Physical Objects”, with Prof. S. K. Kokate, Fergusson College, Pune.

Honours and Awards:

1. “Cosmology: Comparative Study of Cosmological Theories and Aspects of Modern Cosmology” (July 2005 - Dec 2005) under supervision of Dr. L. D. Kadam, YCIS, Satara (India), (Received first prize among several undergraduate projects).

2. “Best question award” at Science Conference organized by Vijeta Science Popularisation, Kolhapur, May 2004.

3. Distinction in “4 th National Science Olympiad of Physics ”, February 2002

Educational Qualification:

Degree Board / University Year of Passing

Marks obtained (%)

Class

M.Sc. (Physics/Astrophysics)

Fergusson College, University of Pune, Pune

June 2009 60.3 First Class (A)

B.Sc. (Physics/Astrophysics)

Yashawantrao Chavan Institute of Science, Shivaji University, Kolhapur

June 2006 65.64 First Class (A+)

HSC(Higher Secondary School Certificate)

Maharashtra State Board June 2003 54 Second Class (B+)

SSC(Secondary School Certificate)

Maharashtra State Board June 2001 65.20 First Class (A+)

Computer Knowledge:

Operating Systems: Win 98, Win 2000, Win XP Professional, Vista, Scientific Linux, UNIX.

Languages: C, C+, UNIX, IDL, and Latex.

Software: IRAF, SM, ISOPLOT, MATLAB, MAPPLE, Starry night.

Other Achievements:

1. I have worked as “lecturer of physics for graduation degree at Spicer Memorial College, Pune”, (Sept. 2008- May 2009).

2. “Participated in Summer School organized by IUCAA, Pune”, (May 2009- July 2009)

3. Organized seminars in “Frontiers in Astronomy” organized by ‘Astroclub’, Fergusson College, Pune in collaboration with IUCAA, as one of the programs in International Year of Astronomy; February 2009.

4. Participated in the “Project Competition” in “Quarks-2008” organized by the Dept. of Physics, Fergusson College (http://www.fergusson.edu/ ), Pune, January 2008.

5. Participated in “National Conference on New Horizons in Physics” organized by

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Yashawantrao Chavan Institute of Science, Satara, January 2007.

6. Participated in “Physikia-07”, Physics exhibition organized by the Dept. of Physics, Fergusson College, Pune, February 2007.

7. Given more than “200 Night Sky Observations and seminars” in different areas of Astrophysics at YCIS, and some nearby institutions / colleges, August 2004 – May 2006.

8. Attended “State level seminars on Century of Relativity” organized by Modern College, Vashi at Vashi, December 2005.

9. Certificate course MS-CIT with 86% in self-study mode at KBPIT, Satara (Oct 2005).

10. Established “Space Physics Students Association (SPSA)” at Yashawantrao Chavan Institute Of Science, Satara, August 2004.

Personal Information:

Name: Dhairyashil Hanamantrao Jagadale

Date of Birth: 15th July 1986

Nationality: Indian

Gender: Male

Marital status: Single

Phone No.: + 9 1 2 3 7 5 2 6 3 2 9 5

Mobile No.: + 9 1 9 4 2 1 2 1 3 1 9 5

E-mail Id: dhjagadale@gmail.com

Address: A/P: Budh, Tal: Khatav, Dist: Satara, PIN: 415503

Languages known: Marathi, Hindi, English and German (Basic)

Hobbies: Writing, Reading, Night sky observation, Bird watching and trekking

Declaration: I hereby declare that the above given information by me is true and correct to the best of my knowledge.

Date: 30th, Nov. 2009Place: Pune (India) (Dhairyashil Jagadale)

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Research Experience

The enchanting view of night sky has made me curious about the Universe. This led me to apply for

B.Sc. degree. As a B.Sc. project I have enjoyed an exciting project in “Cosmology: A comparative

study of cosmological theories and aspects of modern cosmology“. Also as another project I

have worked on Photometric Studies of Globular Clusters at YCIS

(http://www.erayat.org/ycis/). Further, in M.Sc. I developed my keen interest in the interplay

between observational Astronomy and theoretical models. As a part of M.Sc. course I have done

my project in ‘‘Star Formation Rates in Spiral Galaxies Against the Background of Galactic

Properties“ at IUCAA (Inter University Center for Astronomy and Astrophysics,

www.iucaa.ernet.in). One of the most important quantitative parameters that characterizes the

ongoing star formation in a galaxy is the star formation rate (SFR), defined as the total mass of the

stars formed per unit time (per unit year). In an effort to study the properties of star formation in

galaxies, we investigate the size and luminosity function of HII regions by using two methods for

photometry (1) HIIphot and (2) Source Extractor (SE). We compare the performance of the two

methods and select best of them to investigate the size and luminosity function of HII regions. HII

regions are in photoionization equilibrium, which means that the number of ionizations caused by

the UV photons with energies greater than 13.6eV is balanced by the number of recombinations.

When the free electrons recombine to form neutral hydrogen, the transition between various energy

levels gives rise to specific emission lines of the hydrogen series, such as Lyman, Balmer, Paschen,

series etc. In this project, we trace the HII regions or the sites of recent star formation by using the

Balmer H-alpha line. As a case study, we used the continuum broad-band (R), and narrowband H-

alpha images of the nearby galaxy NGC6951 (HST image: proposal ID: 9788) to study the

properties of HII regions and to derive the star formation rate. The images were already pre-

reduced using IRAF (Image Reduction and Analysis Facility) and we used them to obtain pure

emission line images. For this we obtained the scale factor or the ratio of Halpha image to the R

band image using pure continuum sources (stars). The R band image is scaled by the corresponding

factor and subtracted from narrow band image to yield the pure Halpha emission image. Further, to

determine the size and luminosity function (LF) of HII regions we used the two photometric

techniques. The first method known as HIIphot is an IDL (Interactive Data Language) code written

by David Thilker and another methode known as Source Extractor. We further find out LF, Size

distribution and mass distibution in the starforming region which directly scale with the star

formation rate. Further, I continued with the research in star formation at IUCAA with another

project entitled: “A Study of Star Formation in Starburst Galaxies”. Starburst phenomenon has been

found to be very dominant at high redshifts and most of the ground based large telescopes and

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space telescopes have an observational programes devoted to the study of star forming galaxies at

intermediate and high redshifts. These observations essentially sample the integrated properties of

the star forming regions. Inorder to understand and interprete the integrated spectra, colors and

luminosities in terms of the IMF, SFR and the ages of the ionising clusters, it is very important to

study nearby starbursts in detail. The work done under this project aims at studying the physical

properties of the nebular gas and the stellar population in a sample of nearby starburst galaxies. The

observational technique includes broad-band BVR and narrow band H-alpha imaging, and optical

NIR spectroscopy. All the observations required for present study were obtained using the 2.34m

Vainu Bappu Telescope at the Vainu Bappu Observatory in kavalur, India. The distribution of the

ionized gas in the galaxies were analysed based on the H-alpha emission morphology and the

distribution of dust was traced using the B/R color maps. The star formation rates for the star

forming regions have been derived from H-alpha luminosities. The ages of the young stellar

population have been determined based on the evolutionary synthesis models. A study of the

statistical properties of HII regions in galaxy NGC 1365 was carried out. We find that the size

distribution can be well fitted by an exponential law. From the steeps of the HII region lumonosity

function and the small characteristics diameters dirived from the size distribution for NGC 1365

and other early type galaxies in the literature, it appears that some dynamical phenomena are

responsible for inhibiting the formation of supergiant HII regions in these galaxies. Further we

hope to find out upper mass limit to IMF.

With these main projects I have been enjoyed two more theoretical projects in Astrophysics; first is

entitled as “Blackhole Entropy as a perceiver of Quantum Gravity” and other is entitled as

“Massive GWs and Their Signature on CMB Polarization Spectrum”.

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Research Interest and Personal Goals

Thus far, I have been enjoying the study of star formation and addapting several new techniques to

move forward toward my goals. However, the three years of my graduation and two years of

master’s program have provided me with a space to ask new questions and delve into understanding

one area in Astrophysics. When I was in first year of master’s degree, on one dark night, I was

observing a supernova. While observing I thought to pull the time in backward direction of

evolution of supernova. At the end I reached to a gaseous cloud of molecular and atomic hydrogen

with some questions like: How stars born from such a gaseous cloud? Is there any upper and lower

limit on mass of newborn stars? Do the stars form in association? Do the process of massive star

formation and low mass star formation differ from each other? What can be the observational

conditions to observe the ongoing star formation? What fraction of clouds forms stars? What can be

the rate of star formation? What can be the impact of star forming regions on their surrounding? All

these questions led me to perceive a master’s project in ‘Star formation’ under guidance of Prof.

Swara Ravindranath at Inter University Center for Astronomy and Astrophysics (IUCAA), Pune

(India).

Even if this is the beginning of my work in the area of ‘star formation’, I expect to continue in this

area for further research. Within this idea, there are a variety of subjects I would like to explore

including the major questionable aspects like: What is the sequence of observable states leading

from molecular clouds to young high and low mass stars? What are the initial conditions of massive

star formation and how do they come about? Do the massive stars always form in dense stellar

clusters or can they form in isolation? What special conditions are necessary to allow mergers of

stars? What clues to the origin can be gleaned from the multiplicity observations? How does the

forming massive star influence its immediate surroundings, possibly limiting its final mass and / or

final mass of its neighbors? How young mass influence their global environment either by

inhabiting or by triggering further star formation? All these questions pique my interest; I realize

that there is so much that I do not know. As I gain more exposure to the field of Astrophysics, there

are many areas that I would like to understand fully.

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Main Goal:

I am strongly motivated toward the understanding of the Initial Mass Function (IMF): Its

origin, upper and lower mass limits, its properties, distribution and eviolution. Are there any

intial conditions for the distribution of IMF so that the low mass star formation would differ

from the high mass star formation? In case of low mass star formation Core Mass Function

(CMF) may resembles the salpeter IMF. But will it true for massive star formation? If CMF

and IMF have are one – to – one relationship then it can also true that the fragmentation

process within a molecular cloud would set the shape of IMF at the early evolutionary stage.

Attempting to this scenario, we can analyze high angular resolution interferrometric

observations of several Massive Star Forming (MSF) regions at millimiter wavelengths,

describing their protostellar content and deriving their CMF whenever is possible.

Another approch toward the understanding of the stellar mass distribution of different

regions can be the comparision of star formation due to CMF and circumnuclear mass. This

approch may be equivallent to the comparision of high and low mass star formation.

Determination of the radiation softness parameter through optical NIR spectroscopy for a

large sample of starbursts would help to understand the metallicity dependence of the stellar

effective temperatures or the upper mass limit on IMF.

I would like to work dedicatively to persue the understanding of IMF and star formation.

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