For corporate researchers we can also follow up directly with your R&D manager, or the information management contact at your company. 121, Universit ´e Paris-Sud, F-91405, Orsay, France 2 Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research (TIFR),

6 0 obj 10-year back file (where available). /��-Tu��s�w����:�Ɨ�')%6�VzE�R�g�J�2A� ǻ,J�PE����:;���g�J������:�2I ��`�?&S���� �(�a� �r�UWhT�)J��b���S�V��6q�)�N�+o�}z*�͠��LEN��� ���P�XUd�R�. ���h����5�­���M����������qĝVo!�ܞQ4�O70�*�P��9�x������at��+��.nϏ?gx���K=�֭�yL㫼�Q:�BV*[�������)L�12�#M��s��P�iٱ�Wml���(�8��a�ud+�� �Xv��2\��V 9�~�2t���w��>��z�K�*���S�'�����ѿ��X�ovV�p�� �v�@�/�O��.8�\r�hn��ܜ:�f|WXa�`�HسNvӡ=�b�n���DC�>��i�}k��H�SzZ.� ��_/M���sC7YѴY{�J�6kڲ���E��}�yG*O&�kD�P��@�C�ܗz�sy�y:�o}_��s�UF����E�q�m�k ]�&�����ޏ. If you have a user account, you will need to reset your password the next time you login. RIS. 2008 IOP Publishing Ltd Find out more. Find out more about journal subscriptions at your site. Published 12 May 2008, Nabila Aghanim et al 2008 Rep. Prog. These CMB secondary anisotropies encode a wealth of information about the distribution of dark matter and gas throughout our universe. To gain access to this content, please complete the Recommendation endobj 10-year back file (where available). ����@��`��Qq�ZlJ'���[ux�p Secondary Anisotropies CMB photons traverse the large-scale structure of the Universe from z ˘1000 to the present Having nearly scale-invariant adiabatic fluctuations (from CMB observations), structures form bottom-up i.e. x��][��q�3��o8O���w`�X�\Nʮ�'e�*I�+.yd�����t�� ����҃N�� �F�����������?y���7Ͽy n�?�����{���G���7Rn�����_�/�W7^�mw7�^=�����ڄS��Mج���uw��[�V���ͧ�q�����(6�}x��:lBY��O��J��?;�̆�=�-a$k�����۟d�g��>�Q�Q��~����O&x�~��U���_�X��4��a ����l.�ϣC�a+���)0V��A��5��{�_�Uv��_!����xk�܄���6�w�? Find out more about journal subscriptions at your site. Reports on Progress in Physics,

management contact at your company. Institutional subscribers have access to the current volume, plus a �3� ��:���y� x;&��@�X��="���'�d!�)�(�"l(�QP� �(����:aw[�X��LwK�uT6�aV���6�@���fZ�0`�J�D/̕K��(���͡dXq���2�p��J@Ϡ�͑Ȗ� ��k�4���#c�A+K�Y�����+�d�p�,�F� �� ����8 �(U���Z���ڙ�\N׃����X4!��!�j���5�Ȏo��Qr�S�o9�u���6nI Please choose one of the options below. The distribution function, fα(r,pν,t), of any radiation field is defined To gain access to this content, please complete the Recommendation

BibTeX Secondary Anisotropies ... • CMB photons scatter off moving electrons, thus fluctuations expected to by polarized at ~10% level. Export citation and abstract Form and we will follow up with your librarian or Institution on your behalf. 2008 IOP Publishing Ltd

The Cosmic Microwave Background fluctuations provide a powerful probe of the dark ages of the universe through the imprint of the secondary anisotropies associated with the reionization of the universe and the growth of structure. The cosmic microwave background radiation and the cosmological redshift-distance relation are together regarded as the best available evidence for the Big Bang theory. We discuss the different signatures arising from the secondary effects in terms of their induced temperature fluctuations, polarization and statistics. rQY�\�YJ��g�a���� You will only need to do this once. *O�=�h Nb���}}ds���E�W����5�{[G�7��u�nC��҆����QMu�~�����K�Z����eOҳ��bѤ�%��A�ٞ8���L����UՕ��V��lA���Y�vu4l�)7�zn>�������=��V�$��[���y�O���� The secondary anisotropies are being actively pursued at present, and we review the future and current observational status. pK�>��Z�71��][�вV5�V.lrYE�2���������\ 孴���1�ctk�[p� �3���5�K�w�8�y��]�5�c-V�G ��JV��4�d�����M^4o\��w*s$��� � The secondary anisotropies are being actively pursued at present, and we review the future and current observational status. Phys. By continuing to use this site you agree to our use of cookies. We review the relation between the secondary anisotropies and the primary anisotropies that are directly generated by quantum fluctuations in the very early universe. BibTeX The computer you are using is not registered by an institution with a subscription to this article. [cG�l-6���M��C��[G���{ia���ے�P�bF�uWT��~��mތQ����5c��#s��Rg��B^!��+��-��쪲��s�^��C�ԑ_="D�'���6��VPG��"���u�Z�X�H�n�|s��Ն:��:��]�$�ם���M���y�u�%����K��Oטav`W�d�6Q��EC�SP�(*��b���������ʶ2�OU�ӑ�\��u��LQb�C��x뤟���"`}�BĨ��� We review the relation between the secondary anisotropies and the primary anisotropies that are directly generated by quantum fluctuations in the very early universe. Published 12 May 2008, Nabila Aghanim et al 2008 Rep. Prog. eUiuP��b���eQ��Q��w���B?k�]G�u>�_&Eb7�&"�K��rX�~둁�zk).��6`�{��ڄIGy����h&�7s���ߧ�IV�ѭo�Sg���k x�/R&�GJ��\?_p���T�>�t�³�24�ƾl�����-Vݜ��0^�P�>4��������U�G>��a��r����̟��q�?h:� J�o�hG��|T3�J��dmiS��6Xt�F.Ցh��֜�F�# Export citation and abstract Reports on Progress in Physics, i�y�����8xLR���1f��S��`I�{[����m��{�-��~9�u�hs>ut>_f� �ze�d?���;�c2H�������!c̺ Ov�~�+ ��ϋ䝃�Ճu�j=� ��1�Y�Cf��@!��,룁p�T�l%0�p-&�P��h���S���}�u��AFj������`����v�V��6��6��:���l���=Dx�r�p���`�-F8T�~pH��k���>ާ��� ��``����>����͢8��8g�Ad��v

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